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SPACE RESEARCH IN SLOVAKIA
2018 – 2019
SLOVAK ACADEMY OF SCIENCES
COSPAR
SLOVAK NATIONAL COMMITTEE
Slovak Central Observatory Hurbanovo
MAY 2020
2
Space Research in Slovakia 2018 2019
National Committee of COSPAR in Slovak Republic
Slovak Academy of Sciences
Editors: Ivan Dorotovič and Ján Feranec
Slovak Central Observatory, Hurbanovo, May 2020
ISBN: 978-80-89998-09-8
3
CONTENTS
1. EXPERIMENTS FOR MEASUREMENTS IN SPACE ……….… 4
J. Baláž, P. Bobík, M. Musilová
2. SPACE PHYSICS, GEOPHYSICS AND ASTRONOMY………….. 13
J. Baláž, P. Bobík, I. Dorotovič, R. Langer, L. Kornoš, Š. Mackovjak,
M. Revallo, J. Rybák, J. Šilha, J. Tóth
3. LIFE SCIENCES ………….…………….………….……...… 35
M. Musilová
4. MATERIAL RESEARCH IN SPACE ……………………...….... 38
J. Lapin
5. REMOTE SENSING………………………………….............. 39
Ľ. Balažovič, I. Barka, T. Bucha, J. Feranec, T. Goga, M. Kopecká, J. Oťaheľ,
J. Pajtík, J. Papčo, P. Pastorek, M. Rusnák, I. Sačkov, M. Sviček, D. Szatmári,
A. Zverková
6. SPACE METEOROLOGY…………..…………………............ 70
J. Kaňák, Ľ. Okon, L. Méri, M. Jurašek
7. PARTICIPATING IN SPACE RESEARCH IN SLOVAKIA.
NATIONAL COMMITTEE OF COSPAR …………..…………. 82
4
1. EXPERIMENTS FOR MEASUREMENTS IN SPACE
J. Baláž, P. Bobík, M. Musilová
Experiment MEP-2 on board of Spektr-R (Radioastron)
The data acquisition from the experiment MEP-2 was terminated on 10th
January 2019 as a result of failure of communication with the Spektr-R spacecraft
due to the spacecraft command receiver malfunction. The mission was anyway
very successful as it was operative on orbit for 7.5 years instead of planned 3
years. The programmable energetic particle spectrometer MEP-2, developed and
constructed at the Department of Space Physics IEP-SAS was operative over
entire mission lifetime and delivered large amount of valuable science data.
Figure 1.1. Energetic particle spectrometer MEP-2. The configuration on delivery and after
installation on board of the space observatory Spektr-R (Radioastron).
The description and on-orbit operation of the PLAZMA-F suite is described in
[1], the MEP-2 experiment is described in [2]. Amid significant results of the
MEP-2 experiment, e.g., a new type of oscillations of energetic ions flux near the
Earth’s bow shock was revealed [3]. This kind of particle flux variability could
be ever observed due to high time resolution and wide energy range of MEP-2
spectrometer.
5
Experiment SERENA/PICAM for mission ESA-BepiColombo
IEP SAS contributed to ESA-BepiColombo mission to planet Mercury in the
frame of scientific-technical cooperation with Space Technology Ireland (STIL)
and Institute for Space Research of Austrian Academy of Sciences (IWF-ÖAW).
The delivery involved the mechanical structures of the PICAM (Planetary Ion
Camera) instrument that were manufactured in Slovakia (mechanical stress
simulations and mechanical components manufacture on 5-axis centre of Q-
Products, Bratislava, space-qualified processing and integration and testing at
IEP-SAS, Košice).
Figure 1.2. SERENA / PICAM and Mercury planetary orbiter (MPO) of BepiColombo mission.
PICAM is a part of a complex space science suite SERENA for particle
detection at planet Mercury, the launch of the mission was on 20th October 2018,
the science payload is operating nominally. The first flyby of planet Earth is
scheduled on March 2020 followed be flyby of planet Venus in October 2020.
The arrival to Mercury is scheduled in 2025. The detailed description of the
PICAM device is provided in [4].
Experiment PEP/JDC for mission ESA-JUICE
Experiment PEP (Particle Environment Package) will provide comprehensive
detection and analysis of the plasma and particle environment in the system of
planet Jupiter and its Galilean moons Europa, Calisto and Ganymede. PEP will
measure density and flux of positive and negative ions, electrons, exospheric
neutral gas, thermal plasma and energetic neutral atoms in the energy range from
<0.001 eV to >1 MeV with full angular coverage. The PEP suite includes six
sensors (JDC, JEI, JoEE, NIM, JNA and JENI) that are under development at
6
several EU and US institutions led by Swedish Institute for Space Physics (IRF,
P.I. prof. S. Barabash). Based on invitation from IRF, the IEP-SAS contributes to
development and construction of anti-coincidence particle detection system for
JDC sensor (Jovian plasma Dynamics and Composition) of the PEP suite. The
anti-coincidence system will improve the plasma particles detection efficiency on
the background of penetrating electron radiation from Jovian radiation belts. The
system consists from silicon solid state detector (SSD) and dedicated processing
electronic unit (ANU).
Figure 1.3. JDC sensor of the PEP science suite and JUICE spacecraft orbiting in the system
of Jupiter and its Galilean moons.
The JUICE mission including the PEP science suite description is described in
[5], the JDC sensor is in details described in [6].
The participation of IEP SAS to JUICE mission is supported by Slovak PECS
(Plan for European Cooperating States) project named: “Slovak contribution to
ESA-JUICE mission: Development of Anti-Coincidence Module ACM for Particle
Environment Package PEP”.
The development, manufacture, testing and calibration of the ACM/EM
(engineering model) were finished in December 2018. The EM unit was then
delivered to IRF Kiruna, Sweden, where it was successfully integrated to the
JDC/EM sensor system.
The flight model (ACM/FM) was built from the space-qualified components
during 2019, the final assembly, testing and calibration was performed in October-
November 2019 at IEP SAS Kosice and the unit was finally delivered to IRF
Kiruna for integration to JDC/FM system.
7
Figure 1.4. (Left) ACM/EM subsystem after integration to JDC/EM at IRF Kiruna. (Right)
ACM/FM under thermal-vacuum test in SPACEVAC space simulator at IEP-SAS Kosice.
Experiment ASPECT-L for project LUNA-26
The experiment ASPECT-L is currently under development at IEP-SAS in
cooperation with Institute for Space Research (IKI-RAN), Moscow, for lunar
mission LUNA-26.
Figure 1.5. Energetic particle spectrometer ASPECT-L for LUNA-26 mission and its position
onboard of the Orbiter spacecraft.
8
The Structural Thermal Model (ASPECT-L/STM) was delivered to IKI-RAN
in 2015, the engineering model of the instrument (ASPECT-L/EM) was delivered
to IKI-RAN in October 2019.
Figure 1.6. ASPECT-L/EM (Engineering Model) as delivered to IKI-RAN, Moscow, Russia, in
October 2019.
Participation of Slovakia in the project JEM-EUSO
JEM-EUSO (Japanese Experiment Module Extreme Universe Space
Observatory) experiment will search for ultra-high energy cosmic rays (UHECR,
with energy above 10^19 eV) by monitoring UV light produced in their
interaction with atmosphere from International Space Station. Department of
Space Physics IEP-SAS works in project frame mainly on UV background model
at the Earth night side. Pattern recognition methods for showers detection in
EUSO experiments measurements are developed at Technical University in
Kosice.
In the UV background model, we focus specifically on identification and
quantification of in the upper atmosphere produced airglow light intensity
variations. The analysis shows the main variations that should be searched in
measurements of the Mini-EUSO experiment operating at ISS since August 2019.
As an important outcome, we present the article Ultra-violet Imaging of the
Night-Time Earth by EUSO-Balloon towards space-based ultra-high energy
cosmic ray observations [7]. This is an article with the analysis of measurements
9
of the EUSO balloon experiment, which took its flight in August 2014. The article
is devoted to the first measurement by a EUSO class detector looking for ultra-
high energy cosmic ray showers from above. The probability of capturing the
shower signal during this flight was not high, the flight served as a technology test
detector and for background measurement, which is a limiting factor in the
observation of showers.
The activities of the IEP SAS group were oriented also on preparing and
building a global network of UV detectors. The UV detector network named
AMON-net is designed for long-term monitoring of the global dynamics of
airglow radiation generation. At present, the network has been in operation and
its main stations have been continuously measuring for more than two years (the
stations in Mexico at the Astronomico Nacional de San Pedro Martir Observatory
and the Canary Islands, Los Muchachos Observatory, La Palma). Other stations
in Germany and the Kolonica Observatory have been measuring continuously for
over a year. Test measurements and control measurements of weeks to months
were carried out in Sweden, the USA, and the Lomnicky Stit. Publication [8]
describing the AMON detector, which is the measuring station for the AMON-
net network. The development of the flight version of the AMON detector is an
ongoing activity. Two test flights were realized at the stratospheric platform
HiDron (www.stratodynamics.ca) in August 2019. First to altitude 30 km, second
to altitude 34 km. A flight version of the detector, AMON (2 pieces) and EMON
(3 pieces) are prepared for NASA EUSO-SPB2 flight, to perform UV background
and light conditions measurements in the main EUSO mission detector.
The evaluation of EUSO-SPB measurements by machine learning methods is
presented in [9]. Analysis of the first measurements from TA-EUSO presents the
ground experiment [10]. Results of calibration measurements of UV light sources
during EUSO flight balloon shows [11].
10
Figure 1.7. HiDron with AMON on CNES balloon before the flight from Timmins, 31. August
2019.
Information regarding the first Slovak satellite skCUBE
The first Slovak satellite skCUBE was designed, developed and successfully
launched into orbit on the 23rd June 2017. The skCUBE project was run by the
Slovak Organisation for Space Activities (SOSA), in collaboration with the
Slovak University of Technology in Bratislava, Technical University in Košice
and the University of Žilina and dozens of companies. In total, over 60 people
volunteered on this project. It was partially funded by the Ministry of Education,
Science, Research and Sport, the Ministry of Transport and the Prime Minister of
the Slovak Republic. In July 2017 the nanosatellite suffered a problem in orbit.
Despite this issue, it continued to transmit data, which were collected by multiple
ground stations all around Slovakia on a daily basis. The satellite functioned
without a restart for 569 days. On the 15th of January 2019, the nanosatellite
stopped transmitting data. A few days prior to this, some parts of the satellite
seemed to be overheating. Members of SOSA attempted to reconnect to the
satellite for several days without success. The project was therefore terminated on
the 1st of February 2019.
11
Data from the satellite are freely available. They are still being processed by
SOSA members and by students from all over Slovakia, Czechia and elsewhere
in the world, who have included them in their bachelors and masters theses. SOSA
also prepared a course open to the public, providing basic information about
receiving and processing satellite data. There was a lot of interest for this course,
which may continue to be provided to students and the public in the future.
Furthermore, the success of the skCUBE project inspired several members of
SOSA and collaborators abroad from Hungary, Japan and the Czech Republic to
prepare a scientific mission called Cubesats Applied for MEasuring and
LOcalising Transients (CAMELOT). Members of SOSA and the skCUBE team
are taking part in the preparation of the CAMELOT nanosatellite fleet hardware.
References:
[1] ZELENYI, L.M. - ZASTENKER, G.N. - PETRUCHOVICH, A.A. -
CHESALIN, L.S. - NAZAROV, V.N. - BALÁŽ, J. - KUDELA, K. -
STRHÁRSKÝ, I. - SLIVKA, M. PLASMA-F Experiment: Three Years of On-
Orbit Operation. In Solar System Research, 2015, vol. 49, no. 7, p. 580-603, ISSN
0038-0946.
[2] BALÁŽ, J. - GLADYSHEV, V.A. - KUDELA, K. - PETRUKOVICH, A.A.
- SARRIS, E. - SARRIS, T. - SLIVKA, M. - STRHÁRSKÝ, I. Energetic Particle
Measurements Onboard Spectr-R with MEP-2. Kosmicheskie Issledovaniya
2013, Vol. 51, No. 2, pp. 100106.
[3] PETRUKOVICH, A.A. - INAMORI, T. - BALAZ, J. - KUDELA, K. -
SLIVKA, M. - STRHARSKY, I. - GLADYSHEV, V.A. - SARRIS, T. -SARRIS,
E. (2015). Oscillations of energetic ions flux near the Earth’s bow shock, J.
Geophys. Res. Space Physics, 120, doi:10.1002/2015JA021077.
[4] ORSINI, S. - LIVI, S. ,..., BALAZ, J. - KUDELA, K., et al. SERENA: A suite
of four instruments (ELENA, STROFIO, PICAM and MIPA) on board
BepiColombo-MPO for particle detection in the Hermean environment. Planetary
and Space Science 58 (2010), pp 166-181, doi:10.1016/j.pss.2008.09.012
[5] http://sci.esa.int/juice/54993-juice-definition-study-report-red-book/
[6] STUDE, J. Advanced Plasma Analyzer for Measurements in the
Magnetosphere of Jupiter. Doctoral Thesis. Swedish Institute of Space Physics
and Umeå University, 2016.
https://www.diva-portal.org/smash/get/diva2:926416/FULLTEXT01.pdf
[7] The JEM-EUSO Collaboration (corresponding authors: MACKOVJAK, Š. -
SHINOYAKI, K.), Astroparticle Physics, 111, 54, 2019
12
[8] MACKOVJAK, Š. - BOBÍK, P. - BALÁŽ, J. STRHÁRSKY, I. PUTIŠ,
M. GORODETZKY, P., Nuclear Instruments and Methods in Physics Research
Section A: Accelerators, Spectrometers, Detectors, and Associated Equipment,
992,150, 2019
[9] VRABEL, M. - GENCI, J. - BOBÍK, P. - BISCONTI, F., 36th ICRC, July
24th-August 1st, 2019 in Madison, WI, U.S.A. Online at https://pos.sissa.it/cgi-
bin/reader/conf.cgi?confid=358, id.456
[10] The JEM-EUSO Collaboration, Astroparticle Physics, Volume 102, p. 98-
111, 2018
[11] The JEM-EUSO Collaboration, Journal of Instrumentation, Volume 13, Issue
05, pp. P05023, 2018
[12] SZABÓ, P. - GOMBÍKOVÁ, K. - FERENCOVÁ, M. - KOŠUDA, M.,
"Keplerian Orbit and Satellite skCUBE," 2019 New Trends in Aviation
Development (NTAD), Chlumec nad Cidlinou, Czech Republic, 2019, pp. 174-
179.
[13] VERTAT, I. - LINHART, R. - Pokorny, M. - MASOPUST, J. - FIALA, P. -
MRAZ, J., "Small satellite ground station in Pilsen experiences with
VZLUSAT-1 commanding and future modifications toward open reference
ground station solution," 2018 28th International Conference Radioelektronika
(RADIOELEKTRONIKA), Prague, 2018, pp. 1-6.
[14] OJUR, B.A., 2019. Low cost and portable software defined radio ground
station (Doctoral dissertation, Engineering and the Built Environment).
[15] BURGER, E. BORDACCHINI, G., 2019. Chronology of Space Activities
in 2017. In Yearbook on Space Policy 2017 (pp. 313-357). Springer, Cham.
Zimmer, P., McGraw, J.T. and Ackermann, M.R., 2019. Optical measurements of
faint LEO RSOs: Cubesats and Fengyun 1C Debris.
[16] SPODNIAK, M. - Semrád, K. - AS AL-RABEEI, S. - MAJCHEROVÁ, N.
- KORBA, P. - HOVANEC, M., "MKP analýza vlastných frekvencií lopatiek
plynovej turbíny motora iSTC-21v." (2019).
[17] BULANOV, D., 2018. Thesis for Doctor’s Degree (Doctoral dissertation,
Chongqing University of Posts and Telecommunications).
[18] ONDREJÁK, M., 2019. Česko a Slovensko v kozmickej ekonomike
(Doctoral dissertation, Masarykova univerzita, Ekonomicko-správní fakulta).
[19] SWARTWOUT, M., 2018. Reliving 24 Years in the Next 12 Minutes: A
Statistical and Personal History of University-Class Satellites.
63 992
13
2. SPACE PHYSICS, GEOPHYSICS AND ASTRONOMY
J. Baláž, P. Bobík, I. Dorotovič, L. Kornoš, R. Langer, Š. Mackovjak,
M. Revallo, J. Rybák, J. Šilha, J. Tóth
The Department of Space Physics, Institute of Experimental Physics, SAS,
Košice (http://space.saske.sk) in collaboration with the laboratories in abroad
continued studies of the dynamics of low energy cosmic rays (CR) and of
suprathermal cosmic particles, as well as high energy cosmic rays based on
measurements in space and on the ground.
Analysis of long term continual measurements by Neutron Monitor at High
Altitude Laboratory of IEP SAS Lomnický štít (LŠ, data in real time available at
http://neutronmonitor.ta3.sk) along with other neutron monitors were used to
confirm correlation between radiation exposures of aircrew members from
selected airline operators registered in the Czech Republic from 1998 up to 2018.
Results of this radiation protection study are presented in [1].
Thunderstorm ground enhancements (TGEs) of secondary cosmic ray fluxes,
recorded by the SEVAN detector system, are compared with simultaneous
measurements of electric field at the mountain top and on its slope at the
observatory of Skalnaté Pleso from May to September in 2017 and from May to
October in 2018
Observation of the processes in Earth's magnetosphere by means of energetic
neutral atoms (ENA) continues by analysis of data obtained by Neutral atom
imaging detector NUADU [2]. The device was constructed at the Institute of
Experimental Physics in collaboration with Space Technology Ireland, Swedish
Institute of Space Physics, Chinese National Space Science Center and operated
on board of the Double Star TC2 spacecraft [3]. Although the TC2 spacecraft was
injected to high apogee orbit, its perigee in range 500 - 800 km also allowed close
up observations at low altitudes in polar region where energetic ion precipitation
take place. The novel analyses has concentrated to emissions of low-altitude ENA
during magnetospheric substorms and showed that the best way to observe
dynamics of magnetospheric ring current variations is from a low orbit spacecraft.
It was shown that the closer the imaging device is to the ENA emission source,
the higher temporal and spatial resolution data can be obtained. In the substorm
expansion phase, magnetic field stretching tailward causes the ion deposition due
to the pitch angle diffusion of RC ions. During the substorm recovery phase,
magnetic field di-polarization with the energetic ion injection at night
accompanied by precipitating ions caused by the pitch angle diffusion at dusk.
This was demonstrated for the first time at a temporal resolution of one minute.
Within the studies of Sun-Earth relations, we have concentrated on the research
of a faint light in the altitudes 80 - 300 km, called airglow. The airglow is not a
well-explored phenomenon. To determine the response of airglow production to
disturbances of the magnetosphere for ground measurements. The result is a
14
publication [4] with an estimation of the decrease in airglow intensity depending
on the degree of magnetosphere disturbances described by the Dst index for
selected positions on the Earth's surface. These are observatories with suitable
meteorological conditions and a series of positions along the auroral boundary for
a highly disturbed magnetosphere (Kp = 8). The second area was the evaluation
of UV background measurements from the EUSO balloon flight in 2014. This
activity was a continuation of the work of previous years published in the article
[5] in 2018 with the conclusions of the analysis. Characterization of its influence
on the detection of extensive air showers, where it acts as a background, is just in
the beginning. Therefore, we have started our own program of airglow monitoring
with one-pixel detectors [6]. This program is supported by the government of
Slovakia through an ESA (European Space Agency) contract under the PECS
(Plan for European Cooperating States).
References:
[1] KUBANČÁK, J. - KYSELOVÁ, D. - KOVÁŘ, I. - HLAVÁČOVÁ, M. -
LANGER, R. - STRHÁRSKY, I. - KUDELA, K. - DAVÍDKOVÁ, M. - PLOC,
O. Radiation Protection Dosimetry, Volume 186, Issue 2-3, December 2019,
Pages 211214, https://doi.org/10.1093/rpd/ncz204
[2] LU, L. - McKENNA-LAWLOR, S. - BALÁŽ, J. Close up observation and
inversion of low-altitude ENA emissions during a substorm event. Sci. China
Earth Sci. 62, 1024-1032 (2019). https://doi.org/10.1007/s11430-018-9307-x
[3] McKENNA-LAWLOR, S. - BALÁŽ, J. - STRHÁRSKÝ, I. - BARABASH,
S. - BRINKFELDT, K. - LI, L. - SHEN, C. - SHI, J. - ZONG, Q. - KUDELA, K.
- FU, S. - ROELOF, E. C. - son BRANDT, P. C. - DANDOURAS, I. The energetic
NeUtral Atom Detector Unit (NUADU) for China’s Double Star Mission and its
calibration. Nucl Inst Method Phys Res Sect A, 2004, 530: 311-
322. https://doi.org/10.1016/j.nima.2004.04.244
[4] PUTIŠ, M. - BOBÍK, P., - MACKOVJAK, Š.: 2018, Method for analysis of
the effect of geomagnetic disturbances on Ultraviolet airglow intensity.
Earth and Space Science, 5, 790800. https://doi.org/10.1029/2017EA000358
[5] The JEM-EUSO Collaboration (corresponding authors: Mackovjak, Š. &
Shinozaki, K.): 2019, Ultra-violet imaging of the night-time earth by EUSO-
Balloon towards space-based ultra-high energy cosmic ray observations,
Astroparticle Physics, 111, 54. https://doi.org/10.1016/j.astropartphys.2018.10.008
[6] MACKOVJAK, Š. - BOBÍK, P. - BALÁŽ, J. - STRHÁRSKÝ, I., PUTIŠ, M.
- GORODETZKY, P.: 2019, Airglow monitoring by one-pixel detector, Nuclear
Instruments and Methods in Physics Research Section A: Accelerators,
Spectrometers, Detectors, and Associated Equipment, 992, 150.
https://doi.org/10.1016/j.nima.2018.12.073
15
The Faculty of Mathematics, Physics and Informatics, Comenius University,
Bratislava was involved in the following eight directions of research as listed
below.
Photometric observations and research of asteroids at Astronomical and
Geophysical Observatory Modra, Faculty of Mathematics, Physics and
Informatics, Comenius University in Bratislava
The photometric program of asteroid observations continued at Astronomical
and Geophysical Observatory in Modra, Comenius University in Bratislava, some
of the projects also in collaboration with the Astronomical Institute of the Czech
Academy of Sciences, Ondřejov, Czech Republic.
In [1] we studied the membership, size ratio and rotational properties of 13
asteroid clusters consisting of between 3 and 19 known members that are on
similar heliocentric orbits. By backward integrations, we confirmed their cluster
membership and estimated times elapsed since separation of the secondaries from
the primary that are between 105 and a few 106 years. By using photometric
observations we derived the accurate absolute magnitudes of primaries and
rotation periods for all the clusters. We found that 11 of the 13 clusters follow the
same trend of primary rotation period vs. mass ratio as revealed by Pravec et al.
(2010).
The spin states of Non-Principal Axis (NPA) rotators offer significant clue to
the evolutionary processes of these asteroids because their excited spin states are
thought to be caused by internal and/or external forces in the past. Incorporating
the photometric datasets obtained from the three apparitions, 2006, 2016 and
2017, we constructed its spin state and shape model of Krylov [2]. We found that
the asteroid is rotating in Short Axis Mode (SAM) with rotation and precession
periods of 68.15 h and 396.30 h, respectively. The largest and intermediate
principal inertia moments are nearly the same: Ib/Ic = 0.98. However, the smallest
principal inertia moments is less than the half of the others: Ia/Ic = 0.23. We
outlined the possible evolutionary processes which led to the observed spin state.
We conducted a photometric, spectroscopic, and dynamical study of V-type
asteroids outside the Vesta family in the inner main belt [3]. The aim was to find
traces of once existing differentiated planetesimals other than Vesta, to provide
the missing observational evidence for theories predicting an abundance of such
planetesimals in the early solar system.
In [4] we presented the study of a sample of 93 asteroid pairs that are on highly
similar heliocentric orbits. We estimated times elapsed since separation of pair
members that are between 7×103 yr and a few 106 yr. With photometric
observations, we derived the rotation periods P1 for all the primaries and a sample
of secondaries. For a part of the studied pairs, we refined their WISE geometric
albedos and collected or estimated their taxonomic classifications. For 17 asteroid
pairs, we also determined their pole positions. Moreover, we found that the
16
primaries of 13 asteroid pairs in our sample are actually binary or triple systems,
i.e., they have one or two bound, orbiting secondaries. We compared the obtained
asteroid pair data with theoretical predictions and discussed their implications.
We found that 86 of the 93 studied asteroid pairs follow the trend of primary
rotation period vs mass ratio that was found by Pravec et al. (2010). Of the 7
outliers, 4 are high mass ratio pairs that were unpredicted by the theory of asteroid
pair formation by rotational fission. The 13 asteroid pairs with binary primaries
are particularly interesting systems that place important constraints on formation
and evolution of asteroid pairs.
Meteor observations and analyses by AMOS network
In 2018-2019 continued the monitoring of meteor activity above the Central
Europe, Canary Islands, Atacama desert in Chile and Hawaii by All-sky Meteor
Orbit System (AMOS), autonomous video observatory for detection of transient
events on the sky. Hardware and software of AMOS have been developed and
constructed at the Astronomical and Geophysical observatory of Comenius
University in Modra.
We introduced and demonstrate the capability of the updated All-Sky Meteor
Orbit System (AMOS) (called AMOS-Spec) [5] to measure the emission lines
intensites of meteoric element abundances of meteors. The AMOS-Spec program
has been created with the intention of carrying out regular systematic
spectroscopic observations. At the same time, the meteoroid trajectory and pre-
atmospheric orbit are independently measured from data collected by the AMOS
camera network. This, together with spectral information, allows us to find the
link between the meteoroid and its parent body, from both dynamical and physical
consideration. Here we report results for 202 selected cases.
Figure 2.1. Distribution of spectral classes identified within the sample of 202 meteoroids in
the mm to dm size range.
17
Figure 2.2. Ternary diagram displaying the spectral classification of 202 meteors of -1 to -14
abs. mag. (corresponding to meteoroids of mm to dm sizes) observed by the AMOS-Spec system
during 20132017 from AGO Modra Slovakia.
Development of Slovakian optical sensor for space debris objects cataloguing
and research
The Department of Astronomy which is part of the Faculty of Mathematics,
Physics and Informatics of Comenius University in Bratislava, Slovakia (FMPI
CU) won an ESA PECS Slovakia activity with a main goal to transform a 0.7-m
Newton telescope (AGO70) dedicated to amateur astronomical observations to a
professional optical system for regular support of the space debris tracking and
research [6]. The development started with the telescope installation at the FMPI’s
Astronomical and Geophysical Observatory in Modra, Slovakia (AGO) in
September 2016. It was necessary to adapt the low-level telescope control to the
needs of space debris tracking. For the image processing software we have chosen
a modular design. It contains several individual elements performing tasks such
as objects search on the frames, centroiding, astrometric reduction and tracklet
building. The observation planning has been developed focusing on Low Earth
Orbits (LEO) up to Geosynchronous Earth Orbits (GEO). The output products
delivered by the system are astrometric positions in international formats (CCSDS
TDM and MPC), light curves and relative color indices obtained by using
Johnson-Cousins BVRI filters.
Fully operational AGO70 system will support cataloguing efforts of the
European partners, which are maintaining their own space debris catalogues for
research and space surveillance and tracking purposes. AGO70 shall support the
tracking of LEO debris by the Satellite Laser Ranging (SLR) stations. In case of
contingencies during ESA satellite missions, e.g., when the spacecraft is not
responsive, a dedicated observation campaign can be performed with AGO70 to
exam the integrity status of the affected spacecraft, to monitor its attitude motion
state and to improve the object’s orbital information.
18
Figure 2.3. AGO70 telescope installed at the Astronomical and Geophysical Observatory in
Modra, Slovakia (left) and light frames acquired with GEO (top right) and LEO tracking (top
bottom).
References:
[1] PRAVEC, P. - FATKA, P. - VOKROUHLICKÝ, D - SCHEERES, D. J. -
KUŠNIRÁK, P. - HORNOCH, K. - GALÁD, A. - VRAŠTIL, J. - PRAY, D. P. -
KRUGLY, YU. N. - GAFTONYUK, N. M. - INASARIDZE, R. YA. -
AYVAZIAN, V. R. - KVARATSKHELIA, O. I. - ZHUZHUNADZE, V. T. -
HUSÁRIK, M. - COONEY, W. R. - GROSS, J. - TERRELL, D. - VILÁGI, J. -
KORNOŠ, L. - GAJDOŠ, Š. - BURKHONOV, O. - EHGAMBERDIEV, SH. A.
- DONCHEV, Z. - BORISOV, G. - BONEV, T. - RUMYANTSEV, V. V. -
MOLOTOV, I. E.: Asteroid clusters similar to asteroid pairs. Icarus, 2018,
Volume 304, p. 110-126.
[2] LEE, H.-J. - DURECH, J. - KIM, M.-J. - MOON, H.-K. - KIM, CH.-H. -
CHOI, Y.-J. - GALAD, A. - PRAY, D. - MARCINIAK, A. - KAPLAN, M. -
ERECE, O. - DUFFARD, R. - KORNOS, L. - GAJDOŠ, Š. - VILAGI, J.: Spin
State of (5247) Krylov. American Astronomical Society, DPS meeting #50, 2018,
id.414.10
[3] MARCINIAK, A. - OSZKIEWICZ, D. - TROIANSKYI, V. - FOHRING, D.
- KWIATKOWSKI, T. - SKIFF, B. - GEIER, S. - BORCZYK, W. -
MOSKOWITZ, N. - GALAD, A. - KANKIEWICZ, P. - KLUWAK, T. -
GAJDOŠ, Š. - VILAGI, J. - POLČIC, Ľ. - WILAWER, E.: Investigating V-type
19
asteroids outside Vesta family. EPSC-DPS Joint Meeting 2019, held 15-20
September 2019 in Geneva, Switzerland, id. EPSC-DPS2019-1379
[4] PRAVEC, P. - FATKA, P. - VOKROUHLICKÝ, D. - SCHEIRICH, P. -
ĎURECH, J. - SCHEERES, D. J. - KUŠNIRÁK, P. - HORNOCH, K. - GALÁD,
A. - PRAY, D. P. - KRUGLY, YU. N. - BURKHONOV, O. - EHGAMBERDIEV,
SH. A. - POLLOCK, J. - MOSKOVITZ, N. - THIROUIN, A. - ORTIZ, J. L. -
MORALES, N. - HUSÁRIK, M. - INASARIDZE, R. YA. - OEY, J. -
POLISHOOK, D. - HANUŠ, J. - KUČÁKOVÁ, H. - VRAŠTIL, J. - VILÁGI, J.
- GAJDOŠ, Š. - KORNOŠ, L. - VEREŠ, P. - GAFTONYUK, N. M. -
HROMAKINA, T. - SERGEYEV, A. V. - SLYUSAREV, I. G. - AYVAZIAN,
V. R. - COONEY, W. R. - GROSS, J. - TERRELL, D. - COLAS, F. - VACHIER,
F. - SLIVAN, S. - SKIFF, B. - MARCHIS, F. - ERGASHEV, K. E. - KIM,
D.-H. - AZNAR, A. - SERRA-RICART, M. - BEHREND, R. - ROY, R. -
MANZINI, F. - MOLOTOV, I. E.: Asteroid pairs: A complex picture. Icarus,
2019, Volume 333, p. 429-463.
[5] MATLOVIČ, P. TÓTH, J. RUDAWSKA, R. KORNOŠ, L. -
PISARČÍKOVÁ A.: Spectral and orbital survey of medium-sized meteoroids,
A&A 629, A71 (2019)
[6] ŠILHA, J. - KRAJČOVIČ, S. - ZIGO, M. - ŽILKOVÁ, D. - ZIGO, P. -
ŠIMON, J. - TÓTH, J. - KORNOŠ, L. - SETTY, S. - FLOHRER, T. - JILETE,
B.: Development of the Slovak 70-cm Optical Passive System Dedicated to Space
Debris Tracking on LEO to GEO orbits, Proceedings of the Advanced Maui
Optical and Space Surveillance Technologies Conference, held in Wailea, Maui,
Hawaii, September 17-20, 2019, Ed.: S. Ryan, The Maui Economic Development
Board, id.85
20
In the Earth Science Institute of the Slovak Academy of Sciences, Bratislava
and Hurbanovo, a number of issues concerning space weather were investigated
and ground magnetic field measurements were performed.
Theoretical studies were devoted in particular to the mechanisms of severe
magnetic stoms with the use of historical magnetograms recorded long time
before the space age. Owing to geomagnetically induced currents, extreme mid-
latitude geomagnetic disturbances might cause serious damages to some
vulnerable technological systems. A part of the space weather research has
therefore to be focused on deeper understanding of the origins and mechanisms
of these phenomena. In [1], three cases of mid-latitude geomagnetic variations
are presented. One of them is a typical mid-latitude magnetic storm. The other
two cases then represent a phenomenon, which is well known in polar and sub-
polar regions; however, it is less common in mid-latitudes. As this phenomenon
can sometimes be very intensive also at mid-latitudes and it can exhibit rapid
temporal changes of the geomagnetic field, it must not be underestimated. In [2],
the extreme magnetic storms are discussed to possibly caused be auroral
ionospheric currents or electric currents parallel to magnetic induction lines. The
study relies on magnetic observations storms from the modern digital era and also
uses the historical magnetograms.
Recently, a new insight into the mechanism of the Carrington magnetic storm
was published, which identified the field aligned currents as the main cause of
this well-known event. The new idea seems to be a promising alternative to the
generally accepted theory, in which the ring current is the main cause of the low-
and mid-latitude magnetic storms. In [5], some records of rapid mid-latitude
magnetic storms are shown. Most of them were recorded by historical magnetic
observatories (years 1837, 1848, 1872, 1918). The profiles of the horizontal
component show that, instead ofthe ring current, the substorm-related current
system probably played an important role in the development of these interesting
geomagnetic variations.
Historical magnetograms recorded in Clementinum (Prague) and reported
previously in yearbooks were collected and prepared for future applications [3].
Daily magnetic observations at the Prague Astronomical Observatory started 180
years ago, on 1st July 1839. The observatory was equipped with standardized
instruments developed by Gauss and Weber at Observatory of Goettingen. The
observations were carried out manually, at the beginning the measurements were
performed more than ten times per day but later the number of the daily
observations decreased to five. Having been a part of Goettingen Magnetic Union,
however, the sampling interval of readings from magnetometers was shortened to
5 minutes during appointed days. Even more dense measurements were carried
out during periods of strong magnetic disturbances. As the results were printed in
yearbooks Magnetische und meteorologische Beobachtungen zu Prag, no
measured data were lost. Absolute measurements reported in the yearbooks are
21
sufficient for reliable reduction of declination. The Prague series of annual means
of declination is the longest continuous series in the 19th century. The data are thus
fully reliable for the study of geomagnetic activity and space weather applications,
which will be demonstrated for a remarkable geomagnetic event recorded in
Prague on 17th November 1848.
Figure 2.4. The variations of the horizontal intensity and declination that were recorded at the
Clementinum observatory on 17 November 1848. The additional time axis at the top of the
figure shows the magnetic local time (MLT).
Some recent studies point out that currents related to the auroral oval,
electrojets and field aligned currents (FACs), are serious candidates for the
mechanism of the intense mid-latitude magnetic storms. It is interesting to re-
analyse historical data under the light of this modern knowledge. In this aim, two
intense magnetic storms are analysed in [4] that were recorded by observatories
Clementinum (Prague) and Greenwich on 17 November 1848 and 4 February
1872, respectively. The latter has been marked as an extraordinary event by
several authors, in particular in connection with auroras. The former (Fig.2.4.),
however, has been little known in the space weather community. Both these
events possessed swift and extensive variations of the horizontal (H) component
(>400 nT and >500 nT, respectively) and were accompanied by auroras sighted
at very low magnetic latitudes. This implies that the auroral oval on the north
hemisphere was vastly extended southward. The variations of the magnetic
declination also indicate that during these events the auroral oval was situated at
magnetic latitudes lower than those of the observatories. The storms studied in
this paper occurred at different magnetic local times (MLTs), ~23 MLT (Fig 2.5.)
and ~19 MLT. Therefore, they might represent mid-latitude events related to
different parts of the auroral oval. In this paper, the H-variation recorded at
22
Clementinum in 1848 is interpreted to be a substorm due to the ionospheric
substorm electrojet. The Greenwich event registered in 1872 then seems to be a
combination of the ring-current storm with a positive variation of the H-
component caused by the eastward electrojet. Both the events of 1848 and 1872
appear to exemplify phenomena that are common in high magnetic latitudes but
which may occasionally happen also at mid-latitudes.
Figure 2.5. The schematic sketch of the conditions of the Clementinum observatory during the
magnetic storm on 17 November 1848. The circles with dots in their centres indicate the
location of the upward FAC, the circle with a cross mark the position of the downward FAC.
The intensity of the electric currents is expressed by means of the boldness of the markers. The
dashed lines represent the lines of force of the magnetic field generated by the FACs. The ΔD
sign stands for the deviation of the magnetic declination. It is supposed that the substorm
electrojet then flowed at a magnetic latitude which was lower than the magnetic latitude of
Clementinum.
Hurbanovo Geomagnetic Observatory of the Earth Science Institute of the
SAS, is located at geographical latitude 47.87° and geographical longitude 18.18°.
It performs continuous monitoring and registration of the geomagnetic field
components. The one-minute mean values of all components of the geomagnetic
field as well as the records acquired with the one-second sampling interval are
available. K-indexes characterising the geomagnetic activity in the middle
latitudes are computed regularly. Main equipment of the observatory includes the
digital variometer station TPM made in Poland (1996) and magnetoregistration
device DI-fluxgate Magson gained on the co-operation bases withGeo Forshung
Zentrum Potsdam and VW Stiftung. For absolute geomagnetic measurements, the
DI-fluxgate magnetometer and proton precession magnetometer ELSEC are
employed. The magnetovariational data in the one-minute step are supplied via
the internet to the INTERMAGNET centre. The data are sent to World Data
Centers in Edinburgh and Paris, from where they are available for the whole
geomagnetic and space weather community. The data are published also on the
CD-ROMs prepared in the frame of INTERMAGNET. That is beacuse the
Hurbanovo Geomagnetic Observatory of the Earth Science Institute of the SAS is
23
a member of INTERMAGNET, the international network of world first order
magnetic observatories. Information about the geomagnetic activity is also
published on the web site of the observatory, www.geomag.sk. The level of the
geomagnetic activity si reported to public media (TV), too.
The members of the Hurbanovo Geomagnetic Observatory staff regularly
perform field measurements at the observation points of the national magnetic
repeat station network, which is a part of the European repeat station network.
The measurements are coordinated by the MagNetE Group. Measurements of the
magnetic declination are performed regularly at selected Slovak airports.
The knowledge of the distribution of the geomagnetic field elements over a
country is important for many practical as well as scientific reasons. Such
distributions result from magnetic surveys. The surveys need to be repeated
periodically: two-year period has been agreed for repeat stations by the MagNetE
Group. This periodicity enables to find out information about the magnetic secular
variations. The last repeat station survey was carried out in Slovakia in 2018.
References:
[1] VALACH, F. - VÁCZYOVÁ, M. Extrémne magnetické poruchy v
pozorovaniach Hurbanovského observatória. In Zborník. X. medzinárodnej
vedeckej konferencie Univerzity J. Selyeho. Webové aplikácie vo vzdelávaní.
Komárno: Univerzita J. Selyeho, 2018, s. 78-85. ISBN 978-80-8122-251-1.
[2] VALACH, F. - HEJDA, P. - REVALLO, M. - BOCHNÍČEK, J. Aký je
mechanizmus extrémnych magnetických porúch v stredných šírkach. In
DOROTOVIČ, Ivan. Zborník referátov z 24. celoštátneho slnečného seminára,
Kežmarok 2018. - Hurbanovo: Slovenská ústredná hvezdáreň Hurbanovo, 2018,
ISBN 978-80-89998-01-2.
[3] HEJDA, P. - VALACH, F. - REVALLO, M. What can be learned from
geomagnetic observations at Prague Observarory (1839-1917): abstract:
IUGG19-0281. In 27th IUGG General Assembly-Assemblée Générale de
L´UGGI: abstracts. - Montreal: IUGG General Assembly, 2019.
[4] VALACH, F. - HEJDA, P. - REVALLO, M. - BOCHNÍČEK, J. Possible role
of auroral oval-related currents in two intense magnetic storms recorded by old
mid-latitude observatories Clementinum and Greenwich. In Journal of Space
Weather and Space Climate, 2019, vol. 9, p. A11.
[5] VALACH, F. - HEJDA, P. - BOCHNÍČEK, J. - REVALLO, M. -
VÁCZYOVÁ, M. Rapid mid-latitude magnetic storms recorded by old
observatories. In Conrad Observatory Journal: IAGA Workshop 2018, 2019,
special issue no. 5, p. 38.
24
In the Slovak Central Observatory (SCO) in Hurbanovo (http://www.suh.sk),
a number of activities related to space research were performed. We observed
sunspots (the Wolf number data were submitted to the SILSO in Brussels,
Belgium and to the SONNE Netz in Germany) and prominences (images are
published at the website of the Observatory). We performed also spectrographic
observations of the solar spectrum (variations of selected spectral lines during a
solar activity cycle) using a horizontal solar telescope with spectrograph, we
registered solar radio bursts using a solar radio spectrometer CALLISTO and
impact of solar flares on the Earth’s ionosphere using a SID monitor. The research
activities comprise study of the:
- differential rotation of the solar corona, automatic detection and tracking of
the sunspots and the coronal bright points,
- automatic detection of the chromospheric plages,
- asymmetry of the north and south hemispheric solar activity.
One researcher from the SCO is the national ISWI (International Space
Weather Initiative, http://iswi-secretariat.org) coordinator for the Slovak
Republic and since September 2014 he is also as a Scientific Discipline
Representative of the SCOSTEP for the field of solar physics. He is member of
the National Committee of the SCOSTEP and chair and representative to the
COSPAR.
We continued to publish at the website of the SCO data on the modified coronal
index (MCI) and the modified homogeneous data set (MHDS) of coronal
intensities based on satellite EUV measurements as a replacement of ground-
based coronagraphic observations at Lomnický Štít. Both the MCI and the MHDS
data sets can be used further for studies of the coronal solar activity and its cycle.
These data are available at http://www.suh.sk/online-data/modifikovany-
koronalny-index and http://www.suh.sk/online-data/modifikovany-homogenny-
rad, respectively.
In the Computer Intelligence Group (CA3) of the CTS/UNINOVA (Caparica,
Portugal) has been developed in previous years a software tool for automatic
tracking of solar activity features (sunspots and coronal bright points - CBPs)
using a hybrid algorithm combining PSO (Particle Swarm Optimization) and
Snake algorithms and recently an image segmentation algorithm, respectively, for
detecting and tracking of a feature, and determining the differential rotation of the
Sun. In [1] we applied a segmentation algorithm called Gradient Path Labelling
(GPL), used originally to identify drusens in medical retinal images, to detect and
track the coronal bright points (CBPs) using images from the AIA instrument
onboard the SDO satellite. Individual measurements of rotational velocity in
respect to latitude are depicted in Fig. 2.6. The CBPs have a tendency to change
shape and size along time, to disappear and reappear at a corresponding
heliographic position, therefore, decision trees were also included in the tracking
solution. Since our CBP detection algorithm uses an active region mask to filter
25
out the CBPs, whose centroid is inside the active regions, the number of
identifications clearly depends on the level of solar activity. Our approach uses
the commonly applied fitting relation to the latitudinal dependence of the
rotational velocity, which resulted in calculation of the optimum fit parameters as
well as the Gegenbauer orthogonal polynomial.
Another segmentation algorithm for automatic detection of CBPs developed
using SunPy and OpenCV in Python is described in [2] (Fig. 2.7). An automatic
tool to detect coronal holes (CHs) and to determine solar differential rotation
using CBPs inside and outside the CHs, respectively, is being developed in the
CTS/UNINOVA-CA3 group.
In the SCO we developed also an alternative software tool to estimate the solar
rotational profile based on cross-correlation (CC) method [3]. Rotational velocity
was calculated for each day in the years 2011 2018 from CC maxima of two
consecutive SDO/AIA images with a cadence of 30 minutes taken through the
21.1 nm filter, in a window of in heliographic longitude and 6in heliographic
latitude (241 x 2761 pxs). It was performed only in the rows where the CC
maximum was higher than 0.5 (Fig. 2.8). The calculation of
was repeated
separately for rows that intersect a CBP and for rows without the contribution of
a CBP, respectively. We call these background rows BCGs (Fig. 2.9).
In collaboration with the Observatório Geofísico e Astronómico da
Universidade de Coimbra (OGAUC, Coimbra, Portugal) we developed new
algorithms to detect and track solar activity features, chromospheric plages as test
features. The Ca II K3 spectroheliograms registered in the OGAUC were used to
investigate the evolution of the chromospheric plages activity during the 24th solar
cycle. Research team of the OGAUC created a special tool based on the
segmentation by watershed method combined with other mathematic
morphological operators to detect automatically and analyse the plages and/or
other solar features. Several procedures are applied to achieve the automatic
detection (top-hat transform, hole filling, tresholding, watershed operation,
gradient operation which allows to obtain contours of plage regions). One of the
great potentialities of using mathematical morphology is its power to deal with
the geometry of complex and irregular shapes. More, north-south asymmetry of
the solar activity can be studied using this tool. The results were published in [4]
(Fig. 2.10).
26
Figure 2.6. Individual measurements of rotational velocity in respect to latitude. Thick solid
black line indicates the best fit to these values using the relation
(b) = A + B sin2(b) + C
sin4(b), where
is the rotational velocity and the b is the latitude. Thin dotted black lines mark
the fit uncertainty using the 1-sigma of the A, B, C parameters. The equatorial rotational
velocity is 14°/day. Rotational profiles derived by other authors are showed for comparison.
Figure 2.7. Illustrative result of the segmentation process using the Python tool for detection
of CBPs in the 19.3 nm SDO/AIA image.
27
Figure 2.8. Rotational profile as derived using the CC method, where squares mark the mean
values in 5° sectors and the solid line is the best fit of these values.
Figure 2.9. Profile of sidereal rotation velocity showing BCG data (circles) and CBP data
(crosses). Solid lines show approximations, for o:
= 12.183 sin2 b 1.955 sin4 b and for +:
= 14.642 3.185 sin2 b 0:304 sin4 b.
28
(a) (b) (c)
(d) (e) (f)
Figure 2.10. HMI SDO images showing the polarity of magnetic field: a) original image
acquired on 3 September 2011; b) original image acquired on 10 August 2012; c) original
image acquired on 10 May 2014; d) facular regions of the image of Figure (a); e) facular
regions of image of the Figure (b) and f) facular regions of the image of Figure (c).
The SCO organised in the year 2018 the 24th National Solar Physics Meeting
with participation from abroad. The goal of the Meeting was to present new results
of solar physics and from the field of the space weather (Sun-Earth connections),
to provide overview of present status in selected fields of solar physics,
geophysics, meteorology, and climatology. A separate space was devoted to the
presentation of research results of undergraduate and PhD students of university
and academic departments and also to results of scientific and popularisation
activities of Astronomical Observatories in the Slovak Republic and the Czech
Republic. Invited talks, short contributions and posters covered the following
fields: physical phenomena in the solar atmosphere, solar activity, total solar
eclipses, space weather, geoactivity, meteorological events with solar forcing.
29
References:
[1] DOROTOVIČ I. - COELHO A. - RYBÁK J. - MORA A. - RIBEIRO R.A.
(2018). Gradient Path Labelling Method and Tracking Method for Calculation of
Solar Differential Rotation using Coronal Bright Points, Astronomy and
Computing, Vol. 25, pp.168-175. doi: 10.1016/j.ascom.2018.09.008
[2] DOROTOVIČ I. - COELHO A. - RYBÁK J. - MORA A. - RIBEIRO R.A. -
KUSA W. (2018). Solar Differential Rotation Profile Estimation using Coronal
Bright Points Data Derived from the SDO/AIA Images, Sun and Geosphere,
Vol.13, no.2, p.129-133. doi: 10.31401/SunGeo.2018.02.02
[3] DOROTOVIČ I. - RYBANSKÝ M. (2019). Rotation of Some Solar Coronal
Bright Features as Derived from the Solar Dynamics Observatory/Atmospheric
Imaging Array (SDO/AIA) 21.1 nm Images (for the Years 2011 - 2018), Solar
Physics, Vol. 294, Issue 8, article id. 109, 9 pp. doi: 10.1007/s11207-019-1501-z.
[4] BARATA T. - CARVALHO S. - DOROTOVIČ I. - PINHEIRO F.J.G. -
GARCIA A. - FERNANDES J. - LOURENÇO A.M. (2018). Software tool for
automatic detection of solar plages in the Coimbra Observatory
spectroheliograms, Astronomy and Computing, Vol. 24, s. 70-83.
doi: 10.1016/j.ascom.2018.06.003.
30
The activities of the Astronomical Institute of the Slovak Academy of
Sciences (AISAS), Tatranská Lomnica (http://www.astro.sk), related to COSPAR,
were devoted to research in stellar, solar, and interplanetary physics using
different satellite observations, mainly in the UV, XUV and X-ray spectral
regions. Stellar data of the XMM-Newton, MOST, and Kepler satellites, including
the HST were used for research of various variable stars and start hosting
exoplanets [2-8]. Data of the current SDO, IRIS, STEREO, ACE, and other
satellites were used for solar research mostly focused on solar prominences and
flares. In common, these data were used with the simultaneously acquired data by
the ground-based solar telescopes [9-15]. Topic of the interstellar particles has
been also addressed [1]. Hereby we present some examples of the results obtained
by the AISAS staff.
Observations carried out with the space observatories, the European Space
Agency's (ESA) X-ray Multi-Mirror Mission (XMM-Newton) and the Hubble
Space Telescope (HST), were used to model the spectral energy distribution
(SED) of the classical nova V339 Delphini, which exploded on August 14, 2013
(= nova age 0) [8]. Using our original method of multiwavelength modeling the
nova spectrum, we revealed new striking results: (i) At the nova age of 35 days,
the WD photosphere was oblate in poles and a slow equatorially concentrated
mass-outflow contained dust grains. (ii) From day 35 to 72, the nova significantly
stopped-down the mass-outflow. (iii) On day 100, the co-existence of the strong
dust emission and the luminous high-temperature WD confirmed the disk-like
formation around the WD, where the dust can spend a long time. (iv) Our
modeling revealed highly super-Eddington luminosity of the burning WD lasting,
at least, for the first 100 days of the nova life. Fig. 2.11. shows a sketch for the
nova ejecta as can be inferred from our SED models on days 35 and 100. This
finding represents a new challenge for theoretical modeling of the nova
phenomenon.
The X8.2-class solar flare SOL2017-09-10T16:06 ranks as the second most
energetic flare in the solar cycle 24. This major eruptive event happened at the
western solar limb and triggered a very fast coronal mass ejection followed by
significant space weather and heliospheric effects including a solar energetic
particles event detected also as ground level enhancement. The flare displayed an
extended arcade of flare loops, being detected in the range of temperatures from
X-rays down to cool chromospheric-like plasmas. While hot flare loops with
temperatures of 106 107 K were observed in the EUV channels of the
Atmospheric Imaging Assembly (Fig. 2.12) aboard the Solar Dynamics
Observatory (SDO/AIA), cool loops with temperatures of 104 K were captured by
two UV SDO/AIA channels and also by the ground-based Swedish Solar
Telescope (SST) which made a series of spectral and spectropolarimetric images
of the cool off-limb loops in the spectral line of single ionized calcium Ca II 8542
Å and the hydrogen Balmer line Hβ at 4861 Å (Fig. 2.12.). The article by Kuridze
et al. (2019) [12] reports on inferring the magnetic field strengths of the cool flare
31
loops using the weak-field approximation applied to the Stokes I and V profiles
of the Ca II 8542 Å line. The analysis reveals coronal magnetic field strengths as
high as 350 G at heights up to 25 Mm above the solar limb. These measurements
Figure 2.11. Left: Observed spectrum of the nova V339 Del (in magenta) and its model (black
line). The model consists of the radiation from the WD (blue line), nebula (green) and dust
(gray). Right: Sketch for nova ejecta. The WD pseudophotosphere is in dark-blue, stellar wind
in light-blue, equatorially concentrated outflow with dust in yellow with gray strips and bow
shocks as orange lines. The white array represents stopping-down the wind from the WD
indicated on day 100 of the nova age.
Figure 2.12. SDO/AIA 171 Å and 304 Å images (top panels) of the X8.2 class solar flare loops
on 2017 September 10, 16:29 UT co-aligned with SST/CHROMIS Hβ line core (bottom left
panel) and the composite of Hβ wing images at ± 0.735 Å (bottom right panel).
32
are substantially higher than a number of previous estimates and may have
considerable implications for our current understanding of the extended solar
atmosphere.
How much of the dust population originates locally in the solar system and
how much comes from beyond? How big is the probability that an interstellar
meteoroid passing through the solar system will hit the Earth? How are the speed
measurements by which interstellar meteoroids are identified affected by the
uncertainties of the statistical treatment or measurement errors? These problems
and the presence of a large number of meteoroid orbits determined as hyperbolic
in meteor databases has led to meteor astronomers who deal with particles
registered in the Earth's atmosphere from AISAS and scientists who work with
the dust measured on detectors on board of the space probes working together.
The results, summarized in the chapter „Interstellar Meteoroids“, in a book
published by Cambridge University Press in 2019 [1], showed that, except for two
macroscopic interstellar objects, the only dependable detection of interstellar
particles in our solar system to date are the measurements of interstellar dust
originating from the Local Interstellar Cloud. Not a single case of a meteor
claimed to be produced by an interstellar particle has proven satisfactorily
convincing and not one interstellar fireball has yet been reported.
Researchers from AISAS carried out follow-up observations of targets from
the K2 mission and discovered a unique object, a chemically peculiar Ap-type star
showing δ Scuti pulsations that is bound in an eclipsing binary system with an
orbital period shorter than 3 d [7]. HD 99458 is therefore a complex astrophysical
laboratory opening doors for studying various, often contradictory, physical
phenomena at the same time. It is the first Ap star ever discovered in an eclipsing
binary. The orbital period of 2.722 d is the second shortest among all known
chemically peculiar (CP2) binary stars. Pulsations of δ Scuti type are also
extremely rare among CP2 stars and no unambiguously proven candidate has been
reported. HD 99458 was formerly thought to be a star hosting an exoplanet, but
we definitely reject this hypothesis using photometric observations from the K2
mission and new radial velocity measurements.
Besides of this, the AISAS staff was involved (or leading) in the last two years
in 4 coordinated observing campaigns focused on observations of several aspects
of the solar activity. The integral part of campaigns were also measurements
performed by the space-born instruments on different satellites, e.g. IRIS, SDO.
The measurements were coordinated with the ground-based instruments including
the AISAS owned CoMP-S and SCD instruments at the Lomnicky Peak
Observatory.
33
References:
[1] HAJDUKOVÁ, M., Jr. - STERKEN, V. - WIEGERT, P. Interstellar
meteoroids. Meteoroids: Sources of Meteors on Earth and Beyond. Cambridge:
Cambridge University Press, 2019, p. 235-252.
[2] GAJDOŠ, P. - VAŇKO, M. - PRIBULLA, T. - DUPKALA, D. - ŠUBJAK, J.
- SKARKA, M. - KABÁTH, P. - HAMBÁLEK, Ľ. - PARIMUCHA, Š. Transit
timing variations, radial velocities, and long-term dynamical stability of the
system Kepler-410. Monthly Notices of the Royal Astronomical Society, 2019,
vol. 484, no. 3, p. 4352-4359.
[3] GAJDOŠ, P. - VAŇKO, M. - JAKUBÍK, M. - EVANS, P. - BRETTON, M. -
MOLINA, D. - FERRATFIAT, S. - GIRARDIN, E. - GUDMUNDSSON, S. -
SCAGGIANTE, F. -PARIMUCHA, Š. WASP-92, WASP-93, and WASP-118:
transit timing variations and long-term stability of the systems. Monthly Notices
of the Royal Astronomical Society, 2019, vol. 485, no. 3, p. 3580-3587
[4] GAJDOŠ, P. - VAŇKO, M. - PARIMUCHA, Š. Transit timing variations and
linear ephemerides of confirmed Kepler transiting exoplanets. Research in
Astronomy and Astrophysics, 2019, vol. 19, no. 3, article no. 41, p. 1-6
[5] HAMBÁLEK, Ľ. - VAŇKO, M. - PAUNZEN, E. -SMALLEY, B. T Tauri stars
in SuperWASP and NSVS surveys. Monthly Notices of the Royal Astronomical
Society,2019, vol. 483, no. 2, p. 1642-1654.
[6] PAUNZEN, E. - HANDLER, G. - WALCZAK, P. -HUMMERICH, S. -
NIEMCZURA, E. - KALLINGER, T. - WEISS,W.W. - BERNHARD, K. -
FEDURCO, M. - GÜTL-WALLNER, A. - MATTHEWS, J.M. - PRIBULLA, T.
- VAŇKO, M. - WALLNER, S. - RÓZANSKI, T. A revisit to the enigmatic
variable star 21 Comae. Monthly Notices of the Royal Astronomical Society,
2019, vol. 485, no. 3, p. 4247-4259
[7] SKARKA, M. - KABÁTH, P. - PAUNZEN, E. - FEDURCO, M. - BUDAJ, J.
- DUPKALA, D. - KRTIČKA, J. - HATZES, A. - PRIBULLA, T. -
PARIMUCHA, Š. - MIKULÁŠEK, Z. - GUENTHER, E. - SABOTTA, S. -
BLAŽEK, M. - DVOŘÁKOVÁ, J. - HAMBÁLEK, Ľ. - KLOCOVÁ, T. -
KOLLÁR, V. - KUNDRA, E. - ŠLECHTA, M. - VAŇKO, M. HD 99458: First
time ever Ap-type star as a delta Scuti pulsator in a short period eclipsing binary?
Monthly Notices of the Royal Astronomical Society, 2019, vol. 487, no. 3, p.
4230-4237.
[8] SKOPAL, A. Multiwavelength modeling of the SED of Nova V339 Del:
Stopping the wind and long-lasting super-Eddington luminosity with dust
emission. The Astrophysical Journal, 2019, vol. 878, no. 1, article no. 28,p. 1-18.
[9] DORAN, D.J. - DALLA, S. - ZELINA, P. Temporal evolution of heavy-ion
spectra in solar energetic particle events. Solar Physics, 2019, vol. 294, no. 5,
34
article no. 55, p. 1-26.
[10] HERNANDEZ-PEREZ, A. - SU, Y. - VERONIG, A. -THALMANN, J.K. -
GÖMÖRY, P. - JOSHI, B. Pre-eruption processes: Heating, particle acceleration,
and the formation of a hot channel before the 2012 October 20 M9.0 limb flare.
The Astrophysical Journal, 2019, vol. 874, no. 2, article no. 122, p. 1-11.
[11] KOZA, J. - KURIDZE, D. - HEINZEL, P. - JEJČIČ, S. -MORGAN, H. -
ZAPIÓR, M. Spectral diagnostics of cool flare loops observed by the SST. I.
Inversion of the Ca II 8542 A and H-beta lines. The Astrophysical Journal, 2019,
vol. 885, no. 2, article no. 154, p. 1-13.
[12] KURIDZE, D. - MATHIOUDAKIS, M. - MORGAN, H. - OLIVER, R. -
KLEINT, L. - ZAQARASHVILI, T. V. - REID, A. - KOZA, J. - LOFDAHL, M.
G. - HILLBERG, T. - KUKHIANIDZE, V. - HANSLMEIER, A. Mapping the
magnetic field of flare coronal loops. The Astrophysical Journal, 2019, vol. 874,
no. 2, article no. 126, p. 1-12.
[13] SCHWARTZ, P. - GUNÁR, S. - JENKINS, J. M. - LONG, D. M. -
HEINZEL, P. - CHOUDHARY, D. P. 2D non-LTE modelling of a filament
observed in the H alpha line with the DST/IBIS spectropolarimeter. Astronomy
and Astrophysics, 2019, vol. 631, aricle no. A146, p. 1-12.
[14] VERONIG, A. - GÖMÖRY, P. -DISSAUER, K. - TEMMER, M. -
VANNINATHAN, K. Spectroscopy and differential emission measure diagnostics
of a coronal dimming associated with a fast halo CME. The Astrophysical Journal,
2019, vol. 879, no. 2, article no. 85, p. 1-11.
[15] ZEMANOVÁ, A. - DUDÍK, J. - AULANIER, G. - THALMANN, J.K. -
GÖMÖRY, P. Observations of a footpoint drift of an erupting flux rope. The
Astrophysical Journal, 2019, vol. 883, no. 1, article no. 96, p. 1-13.
35
3. LIFE SCIENCES
M. Musilová
Life sciences research in Slovakia, within the space sector, is primarily
performed by the Slovak Organisation for Space Activities (SOSA) and at the
Faculty of Electrical Engineering and Information Technology of the Slovak
University of Technology in Bratislava (FEI STU), in collaboration with multiple
Slovak and international partners. It is primarily focused on astrobiology and
human space exploration. From an astrobiological perspective, researchers and
students at SOSA and FEI STU study life in extreme environments
(extremophiles) as analogue organisms for the lifeforms that we could potentially
find on other celestial bodies. Part of the research projects focus on the
degradation of biological molecules when exposed to the harsh conditions in the
stratosphere, such as DNA and cell membranes. This is performed by taking
biological samples into the stratosphere using stratospheric balloons developed
by SOSA. SOSA and FEI also have various instruments that can be used to
simulate the atmospheric pressure, temperatures and vacuum at different altitudes.
Extremophiles have also been studied by SOSA and FEI STU in extreme
conditions, such as on the glaciers in Svalbard and within lava tubes on volcanoes
in Hawaii. The former project was based on a collaboration with the University
of South Bohemia (Czech Republic) and the Faculty of Natural Sciences of the
Comenius University in Bratislava (Slovakia). A team from SOSA studied two
different environments in Svalbard, from an ecological, geological and
microbiological perspective and their relevance to extraterrestrial conditions.
Biochemical and genetic analyses were performed on the samples by high school
and university students in Slovakia for educational and outreach purposes.
Students have been studying the survival of these extremophiles in different
simulated planetary conditions and they have used them for their bachelors and
masters projects.
Regarding the human space exploration research, a member of SOSA and visiting
professor at FEI STU has been selected to take part as a Commander of multiple
simulated missions to the Moon and Mars in Hawaii, funded by NASA and ESA.
The research has been focused on both testing the scientific and technological
research that needs to be performed so that humans can return to the Moon and
explore Mars one day. Furthermore, the missions are also aiming to determine
what the ideal types of crewmembers are to send on long duration missions into
space. For these reasons, the missions try to recreate the difficulties and extreme
circumstances of long duration space missions. Then, they assess the performance
of each of the crewmembers individually and how they work as a team together.
These particular missions take place at the Hawaii - Space Exploration Analog
and Simulation (HI-SEAS) habitat, which is located at 2,500 meters in elevation
36
on the active volcano Mauna Loa, on the Big Island of Hawaii. As of 2018, the
International Moonbase Alliance (IMA), an organization dedicated to building
sustainable settlements on the Moon, has been organizing regular simulated
missions to the Moon and Mars at HI-SEAS. The constraints for these missions
depend on which celestial body the mission is simulating to be on. For instance,
for lunar missions the time delay in communications is only of a few seconds, in
comparison to the 20 minute one way delay imposed on communications with
Mars. The crews are supported by a Mission Control Centre based on the Big
Island of Hawaii as well.
In 2019, the EuroMoonMars IMA HI-SEAS (EMMIHS) campaign was
launched at HI-SEAS, bringing together researchers from ESA, IMA, the
International Lunar Exploration Working Group (ILEWG), European Space
Research and Technology Centre (ESTEC), VU Amsterdam and many other
international organizations. During this campaign, two crews spent two weeks
each at HI-SEAS in 2019, performing research relevant to both the Moon and
Mars there. The campaign aims to increase the awareness about the research and
technology testing that can be performed in analogue environments, in order to
help humans become multiplanetary species. Furthermore, the research and
technological experiments conducted at HI-SEAS are going to be used to help
build a Moon base in Hawaii, and ultimately to create an actual Moon base on the
Moon, as part of IMA’s major goals. An example of one of Slovak outreach
experiments on the EMMIHS I mission was a biology project designed by high
school students in Slovakia, as part of a nationwide competition organized by a
member of SOSA and visiting professor at FEI STU. It focused on fertilizing soils
to grow plants on using human hair from the crewmembers during an analogue
mission. Slovak hardware has also been tested at HI-SEAS during missions, such
as the RoboTech Vision rover.
Additionally, SOSA and FEI STU representatives regularly present about the
life sciences research projects that they are working on at multiple international
conferences, including the International Astronautical Congress (IAC) run by the
International Astronautical Federation (IAF) and the Europlanet Science
Congress (EPSC). A member of SOSA and visiting professor at FEI STU is also
a reviewer for the NASA Planetary Protection Research Program and many other
grant programs and research journals in life sciences, such as Astrobiology and
the National Science Foundation. They are an Adjunct Faculty of the International
Space University as well, where they lecture and organise workshops in
astrobiology and the exploration of the Moon and Mars.
37
References:
[1] MUSILOVÁ, M. - ROGERS, H. - FOING, B. (2019) Analogue research performed
at the HI-SEAS research station in Hawaii. Geophysical Research Abstracts, EGU
General Assembly 2019, Vol. 21, EGU2019
[2] MUSILOVÁ, M. - ROGERS, H. - FOING, B. - SIRIKAN, N. - WEERT, A. -
MULDER, S. - POTHIER, B. - BURSTEIN, J. (2019) EMM IMA HI-SEAS campaign
February 2019. EPSC Abstracts, EPSC-DPS Joint Meeting 2019, Vol. 13, EPSC-
DPS2019
[3] ROGERS, H. - MUSILOVÁ, M. - FOING, B. (2019) International MoonBase
Alliance: Goals and Update. EPSC Abstracts, EPSC-DPS Joint Meeting 2019, Vol.
13, EPSC-DPS2019
[4] ROGERS, H. - MUSILOVÁ, M. (2019) How to Live Sustainably on the Moon.
Proceedings of the 70th International Astronautical Congress (IAC) by the
International Astronautical Federation (IAF), 21-25 October 2019 in Washington DC,
USA. Paper IAC-19,A3,2C,11,x52856
[5] SIRIKAN, N. - FOING, B. - MUSILOVÁ, M. - WEERT, A. - POTHIER, B. -
BURSTEIN, J. - MULDER, S. - COX, A. - ROGERS, H. (2019) EuroMoonMars IMA
HI-SEAS 2019 Campaign: An Engineering Perspective on a Moon Base. Proceedings
of the 70th International Astronautical Congress (IAC) by the International
Astronautical Federation (IAF), 21-25 October 2019 in Washington DC, USA. Paper
IAC-19,A3,2C,9,x54636
[6] BURSTEIN, J. - FOING, B. - MUSILOVÁ, M. - ROGERS, H. - SIRIKAN, N. -
MULDER, S. - WEERT, A. - POTHIER, B. (2019) Messaging on the Human
Condition as Space Residents. Proceedings of the 70th International Astronautical
Congress (IAC) by the International Astronautical Federation (IAF), 21-25 October
2019 in Washington DC, USA. Paper IAC-19,A3,2C,9,x54636
[7] WEERT, A. - FOING, B. - MUSILOVÁ, M. (2019). Hydrous alteration of lava
flows on Mauna Loa (Hawaii) compared to Martian volcanic soils. Proceedings of the
50th Lunar and Planetary Science Conference, 1822 March 2019 in The Woodlands,
Texas. 10.13140/RG.2.2.18931.17448/1.
38
4. MATERIALS RESEARCH IN SPACE
J. Lapin
Materials research in space at the Institute of Materials and Machine
Mechanics of the Slovak Academy of Sciences (IMMS SAS) has not been
performed during the period of 2018 2019.
39
5. REMOTE SENSING
Ľ. Balažovič, I. Barka, T. Bucha, J. Feranec, T. Goga, M. Kopecká, J. Oťaheľ,
J. Pajtík, J. Papčo, P. Pastorek, M. Rusnák, I. Sačkov, M. Sviček, D. Szatmári,
A. Zverková
Selected activities of five institutions are included in this report (2018-2019):
Institute of Geography, Slovak Academy of Sciences (IG SAS) in
Bratislava
Project: Advanced Techniques for Biomass Mapping in Abandoned
Agriculture Land Using Novel Combination of Optical and Radar Remote
Sensing Sensors (ATBIOMAP); under the 2nd call European Space Agency
(ESA) the Plan for European Cooperating States (PECS) Slovakia, contract No.
4000123812/18/NL/SC (2018-2020): National Forest Centre (prime contractor),
Zvolen, IG SAS (subcontractor); project link: http://atbiomap.nlcsk.org
Results of identification of agricultural abandoned land (AAL) and land
cover (LC)/land use (LU) classes obtained by the computer-assisted
photointerpretation (CAPI) and object-based image analysis (OBIA)
methods
Agricultural land abandonment is a widespread LU change in different parts
of the Earth´s land surface. This phenomenon is especially notable in countries of
Eastern and Central Europe, where the formerly intensively worked farmland has
been abandoned due to the deep social and political change (disintegration of the
deep socialist agrarian policy, accession to the European Union, increased tele-
connections and joining the global markets).
An example of such changes of agricultural land is Slovakia, where the
abandonment of cultural agricultural landscape has been obvious during recent
almost 30 years. It is a phenomenon perceived in this country as a new social and
landscape-ecological problem. It is also a large-scale issue as the unused area
amounts to approximately 435,000 ha representing 18% of total 2,423,478 ha
farmland in the country.
The theme of mapping the AAL and LC/LU classes by satellite Sentinel data,
biomass quantification and its management is covered by this project.
Attached results (Figs. 5.1, 5.2, 5.3 and 5.4) document the possibilities of the
use of satellite Sentinel data and the CAPI methods, as well as the OBIA in the
process of AAL classes identification in experimental areas of the Podunajská
nížina (PN) lowland and in the Zvolenská kotlina (ZK) basin.
40
Figure 5.1. AAL and LC/LU classes identified by CAPI method in experimental area PN.
Figure 5.2. AAL and LC/LU classes identified by CAPI method in experimental area ZK.
41
Figure 5.3. AAL and LC/LU classes identified by OBIA and Random Forest classifier
in experimental are PN.
Figure 5.4. AAL and LC/LU classes identified by OBIA and Random Forest classifier
in experimental are ZK.
42
Project: Effect of impermeable soil cover on urban climate in the context of
climate change (supported by the Slovak Research and Development Agency
APVV-15-0136); project link:
https://www.vupop.sk/projekty_apvv_15_0136.php
Land cover and its change of Bratislava, Trnava and Žilina for the years
1998, 2007, 2016 obtained by interpretation of satellite data (SPOT, Sentinel
and Formosat)
One of the aims of this project is to document identification and delimitation
of LC/LU classes (Fig. 5.5) and their change (Fig. 5.6) based on Urban Atlas (UA)
data and satellite SPOT, Sentinel and Formosat data in three cities in Slovakia:
the capital Bratislava and two regional centres Trnava and Žilina functional
urban areas (FUAs; located in different geographical conditions) in the years
1998-2007-2016 and their effect on the temperature change by application of the
MUKLIMO_3 model. This model was used in the APVV-15-0136 project for the
purposes of urban heat island modelling. The largest LC/Lu changes were in
benefit of artificial surfaces in FUAs as demonstrated in Fig. 5.6.
Figure 5.5. Spatial distribution of LC/LU classes in the year 2016.
43
Figure 5.6. LC/LU changes between 1986 and 2016.
The long-term co-operation of the Institute of Geography SAS in pan-
European projects CORINE land cover (CLC) resulted in 2018 in the book
publishing: Land cover of Slovakia and its change in 1990-2012 (in Slovak),
160 p. Bratislava, Veda.
CLC data became a valuable source of original information for those
interested in knowing the landscape of European countries and its dynamism. This
monograph (Feranec et al. 2018) document more than 20-year development of
Slovakia’s landscape. Individual parts of the monograph describe CLC projects
regarding the application of satellite data. The methodology of the generation of
four data layers, particularly CLC 1990, CLC 2000, CLC 2006 and CLC 2012, as
well as assessments of their precision and generation of three change layers i.e.
CLCC1990-2000, CLCC2000-2006 and CLCC2006-2012 are demonstrated in an
easy-to-follow manner. Time-spatial characteristics about changes of LC for more
than two decades indicate the increasing trend in deforestation, decreasing trend
in forestation, intensification of agriculture, construction of water reservoirs, and
a mixed trend of the developments in urbanisation, and other changes. Part of the
monograph also brings examples of possible solutions to environmental issues in
Slovakia by application of CLC data. The final part is dedicated to a brief outline
of the prospects for tracking the development of LC in Slovakia in the future in
accord with the European activities in this field.
44
Institute of Geography, Faculty of Science, Pavol Jozef Šafárik University
in Košice
Project: SURGE: Simulating the cooling effect of urban greenery based on
solar radiation modelling and a new generation of ESA sensors (feasibility
study for the European Space Agency; under the 1st call ESA PECS Slovakia,
contract nr. 4000117034/16/NL/NDe, 2016-2018)
Urban greenery has a considerable effect on cooling the urban environment
during heat waves. It is a dynamic component of the urban land cover which can
be observed by the Sentinel 2 (S2) satellite mission in a higher spatial and
temporal resolution than is enabled by other similar missions. The SURGE
feasibility study aimed to explore the potential of S2 multispectral data in
simulating the cooling effect of urban greenery. The main objective was to define
a methodical approach for spatial modelling of land surface temperature based on
modelling the solar irradiation and parameterizing the land cover properties from
S2 data. While solar irradiation can be precisely calculated on a fine scale using
virtual 3D city models other important parameters for land surface temperature
modelling are difficult to ascertain, such as surface thermal emissivity, broad-
band albedo and evapotranspiration. The approach was tested in an area
comprising 4 sq. km of the central part of the Košice City in Slovakia (Fig. 5.7).
Virtual 3D city model of Košice was generated from airborne lidar and
photogrammetric data acquired in a single mission. A time-series of Sentinel 2
data was gathered to be compared with a reference time-series of terrestrial lidar
(TLS) data of urban greenery on 4 small sites. Statistical linear relationship was
defined between the vegetation metrics derived from S2 and TLS data. A
geobotanical database of urban trees was generated based on field survey.
Algorithmic structure of a toolbox for modelling the land surface temperature in
the open-source GRASS GIS was developed based on the Stefan-Boltzmann law
and Kirchhoff rule. This study demonstrated how Sentinel 2 data can be used for
estimating broad-band albedo, land surface emissivity and solar transmittance of
vegetation. The primary benefits are in the developed algorithm for estimating the
land surface temperature in a GIS environment providing a unique platform (i) for
integrating various kinds of datasets to become usable in urban planning and (ii)
for exploiting the S2 data in mitigation of the urban heat island.
45
Figure 5.7. Land surface temperature (LST) modelling for a central area of Košice using Sentinel 2,
terrestrial laser scanning data and GIS tools.
Project: APVV-15-0054: Physically based segmentation of georelief and its
geoscience application (research project supported by the Slovak Research and
Development Agency APVV-15-0054)
Airborne and terrestrial laser scanning and close-range photogrammetry are
frequently used for very high-resolution mapping of land surface. These
techniques require a good strategy of mapping to provide full visibility of all areas
otherwise the resulting data will contain areas with no data (data shadows).
Especially, deglaciated rugged alpine terrain with abundant large boulders,
vertical rock faces and polished roche-moutones surfaces complicated by poor
accessibility for terrestrial mapping are still a challenge. In this project, we present
a novel methodological approach based on a combined use of terrestrial laser
scanning (TLS) and close-range photogrammetry from an unmanned aerial
vehicle (UAV) for generating a high-resolution point cloud and digital elevation
model (DEM) of a complex alpine terrain (Fig. 5.8). The approach is
demonstrated using a small study area in the upper part of a deglaciated valley in
the Tatry Mountains, Slovakia. The more accurate TLS point cloud was
supplemented by the UAV point cloud in areas with insufficient TLS data
coverage. The accuracy of the iterative closest point adjustment of the UAV and
TLS point clouds was in the order of several centimeters but standard deviation
of the mutual orientation of TLS scans was in the order of millimeters. The
generated high-resolution DEM was compared to SRTM DEM, TanDEM-X and
national DMR3 DEM products confirming an excellent applicability in a wide
range of geomorphologic applications (Šašak et al., 2019).
46
Figure 5.8. A workflow of combining terrestrial lidar and photogrammetric point clouds for DEM
production in rugged alpine topography.
Project: TOKAJGIS: Development of webGIS platform based on big-geodata
for the Tokaj Wine Region foster cross-border collaboration (co-financed by the
EU within the programme INTERREG V-A Slovakia-Hungary, contract nr.
SKHU/1601/4.1/052)
The Tokaj wine region may be considered as a unique area from the point of
view of geography, characterized to a large extent by the wine- and viticulture, as
well as the special mining assets close to the national border and a wide variety
of tourist attractions.
The fundamental idea behind the creation of a joint GIS framework by Pavol
Jozef Šafárik University Košice, Slovakia and Eszterházy Károly Univerity Eger,
Hungary was to support the development of the wine region based on the
integration of basic territorial data and the joint handling of GIS by the two
European member states. Databases with different structures and nomenclature
hamper the processing of the GIS data of the wine region, its integration and the
preparation of mutually advantageous regional development concepts as well as
the transparency of developmental efforts.
The aim of the project was to pool the professional experience of the two
institutions and to facilitate joint learning processes based on specific modular
frameworks in keeping with the character of the wine region. The proposed
47
system is capable of integrating the GIS databases present on both sides of the
border and various remote sensing data including cutting-edge UAV and laser
scanning technology (Fig. 5.9 and Fig. 5.10). Furthermore, it deepens the remote
sensing skills and knowledge present at the two institutions. The thematic content
of the trilingual GIS framework published on the website can be used as a
validated source of information for wine producers, local government and
administration, local people as well as the participants (both on the demand and
supply side) of tourism. It provides an easily accessible dissemination platform
on which to publish the research results of the area.
Figure 5.9. The interactive website of the project with remote sensing data
https://geografia.science.upjs.sk/webshared/Laspublish/Tokaj/Tokaj.html.
Figure 5.10. Scout B1-100 UAV with the integrated laser scanning payload (A) and hyperspectral
payload (B). A comprises the VUX-1 laser scanner (Riegl, Austria) (a) and the Sony A6000 E-Mount
photo camera (b). The position and orientation of the sensors is precisely monitored by dual GNSS
antennas (c) and an embedded INS unit xNAV550 (Oxford Technical Solutions Ltd., United
Kingdom) for the sensor attitude and position monitoring. B comprises the AISA Kestrel 10
hyperspectral camera (Specim, Finland) (d) and the INS (c)
48
Activities within the Copernicus Academy
Pavol Jozef Šafárik University in Košice is a member of the Copernicus
Academy network of institutions as the Institute of Geography promotes use of
the Copernicus Services via teaching and research. The Copernicus data are
actively used on practical classes and lectures focusing on Remote Sensing and
Geographic Information Science. We have organized a summer school in July
2018 within the TOKAJGIS project (see above) where the participants were
discussed the benefits of Sentinel 2 and other Earth Observation data in precision
viticulture and farming in general.
49
National Agricultural and Food Centre - Soil Science and Conservation
Research Institute
Remote sensing control of area-based subsidies in agriculture (2018)
The subsidies play a key role in agriculture sector and contribute to the
prosperity of agricultural subjects. The subsidies to agriculture sector represent
major part of European budget and that is why there is taken an emphasis to the
control.
Slovak Administration decided to have six control sites for the 2018
campaign, defined by 710 km2 ANNA, 225 km2 IRMA, 640 km2 JANA, 260 km2
NORA, 371 km2 OLGA and 486 km2 ZORA (Fig. 5.11). Two sites were covered
by WorldView2 images. Two sites were covered by WorldView3 images and two
sites by GeoEye1 images. Two HR acquisition windows were used: HR-1 and
HR+1.
Figure 5.11. Localization of the controlled sites in campaign 2018.
In 2018 campaign the total number of applicants was 18 611, the number of
dossiers controlled with remote sensing was 1125 (6.04% of all dossiers). The
total area controlled was 123,499.78 hectares, with 6477 reference parcels. There
were 28,526 agricultural parcels to control (in 11 schemes), on average 25
parcels/farmer and 109.78 hectare/ dossier.
To determine the agricultural parcel areas, the parcels were located on the
screen with the help of the reference parcel vectors and its limits validated on the
VHR images (WorldView 2 4, GeoEye1 2 images). The agriculture parcels
boundaries were taken as vector data from IS Geospatial aid application IS
GSAA
50
The Fig. 5.12 shows an example of boundary and land use check. Areas, which
are not subsidised like path or stables, are excluded and coded as C6 those are
well visible on the VHR image.
Figure 5.12. Example of boundary check and land use on WorldView4 image.
The land use check with multi-temporal HR images (SPOT 6 images) was
made by computer-assisted photointerpretation (CAPI). The images were overlaid
with the digitized vectors showing the position of the parcels which were checked.
The land use check was completed by Rapid field visits RFVs. As a complement
to control vegetation development, the freely available Sentinel2 satellite images
(resolution 10m/ pixel) were used. The satellite images Sentinel 2 are provided by
ESA.
Areas which are cultivated but the crop haven’t emerged properly or were hit
by some disaster like flood or drought have to be proved on more images from
different acquisition windows (Fig. 5.13).
51
Figure 5.13. Example of land use check on HR images from different acquisition windows.
High resolution (HR) images were corrected to a master image” digital
orthophotomaps with a ground sample distance 0.5 m and declared 1.5 m
RMSExy. Ground control points for VHR images were determined from field
survey post-processed GPS measurement with the use of Slovak spatial
observation system. Ground control points were represented by well defined
points in the build-up area (crossings, path edges in the cemeteries, around the
houses).
The purpose of the remote-sensing control is to check the area and land use of
the agricultural parcels in the dossier. The CAPI is used for checking the area
claimed and generally the land use. The CAPI has been adjusted to the annual
conditions of the regulations of subsidy schemes.
The 2017 campaign is based on Common Technical Specification for the 2018
Campaign of On-The-Spot-checks and area measurement according to art. 24-27,
art. 30, 31 and 34-41 of Regulation (EU) No 809/2014 as amended by Regulation
(EU) 2015/2333 (http://marswiki.jrc.ec.europa.eu) and also is based on agreement
of delegated activities between APA SR and NAFC SSCRI.
According to the final diagnosis, which summarizes the diagnoses of the
conformity and completeness tests at dossier level, 401 (35.64%) dossiers were
accepted for Single area payment scheme, 2 (0.17%) for payment for agri-
environment climate action, 89 (7.91%) for area facing natural constraints, 361
(32.08%) for Complementary National Direct Payment scheme, 3 (0.26%)no
dossier for payments on organic farming, 58 (5.15 %) for payment for agricultural
practices beneficial for the climate and the environment, no dossier for coupled
direct payments for sugar beet and for coupled direct payments for fruit with high
labour inputs, 3 (0.26%) for coupled direct payments for fruit with very high
52
labour inputs, no dossier for coupled direct payments for tomatoes, 1 (0.08%) for
coupled direct payments for vegetables with high labour inputs, no dossier for
coupled direct payments for vegetables with very high labour inputs, for coupled
direct payments for hops and no dossier for Special Areas Of Conservation too.
The declared and retained area on all control zones is compared on Fig. 5.14.
Figure 5.14. Declared and retained area (ha) for schemes CNDPs and SAPS per site.
Quality Assesment of Land Parcel Information System QA LPIS (2019)
Land Parcel Identification System (LPIS) is the main component of Integrated
Administration and Control System (IACS) for land based direct support. The
purpose of LPIS is to implement the common agricultural policy of the European
Union measures. The quality assessment framework of LPIS is an integral part of
LPIS management and upkeep processes. In this framework, the LPIS of a
MS/Region is regarded as a system under test, which is composed of two major
components: the local application schema and the data records stored in the
system. The Executable Test Suite (ETS) targets at the data component by
annually assessing conformity according to Article 6 of (EU) Regulation No
640/2014.
QA implementation is based on current images taken in the year of review.
Selected reference parcels by EC for QA LPIS were on SCRI vectorised on the
background of current satellite images, provided by EC. Subsequently, they are
compared with the valid state of the LPIS layer. The images were overlaid with
the digitized vectors showing the position of the parcels which were checked. The
land use check was completed by Rapid field visits RFVs.
QA LPIS is realized through 9 quality elements, grouped into two conformance
classes, as defined by the Regulation. Based on the item conformance verdicts
53
issued for the various criteria during the item inspection, verdicts made on each
conformance class. There are several reasons for errors. The two most common
are operator error and outdated orthophotomaps.
The conformance class 1 means to “assess the quality of LPIS, and counts
non-conforming items. Furthermore, counting items offers a straightforward entry
for the LPIS upkeep processes. This counting of items includes the first three
types of the quality elements (QE1, QE2 and QE3) (Fig. 5.15).
QE1 assesses the maximum eligible area of the system and evaluates 2 quality
elements: QE1a absence of bias (i.e. accuracy) of the land represented in the LPIS
as a whole, QE1b parcel level precision of the land represented in the LPIS as
a whole overestimation areas and underestimation areas (Fig. 5.16).
QE2 assesses individual parcels with correctness issues and evaluates 3 quality
elements: QE2a proportion of items with incorrectly recorded area or
“contaminated” with ineligible features error type Update outdated
orthophotomaps (Fig. 5.17).
QE2b distribution of items, according to the correctness of the eligible area
recorded and QE2c number of non-conforming reference parcels in LPIS with
classification error mistake/ error of operator (Fig. 5.18).
QE3 shows number of reference parcels that have functional issues "critical
defects" (Fig. 5.16).
Conformance class 2 is assessed under the last three elements (QE4, QE5 and
QE6). QE4 categorization of the non-conformities, QE5 ratio of total declared
area in relation to the total area recorded for the area conforming reference parcels
and QE6 rate of non-conforming reference parcels due to undetected and
unaccounted land cover change, as observed in ETS, accumulated over the years.
These 3 elements aim to "identify possible weaknesses", and this requires a
broader system wide analysis, beyond the individual item or reference parcel. This
is most obvious for QE4 which analyses the LPIS processes and design as factors
for creating quality problems. For instance, a single, large parcel can be
contaminated, can have critical defect (for example, multi-parcel), and can have
its land wrongly classified. Although this represents a single non-conforming
item, it does reflect three different system weaknesses.
Quality assessment of the Slovak LPIS was realized in three zones for
campaign year 2019 (Fig. 5.15). VHR satellite imagery for each zone was
delivered from JRC EC. Site 2019 QA SK 1 cover part of Michalovce district
(EK provided World View 3 satellite image from 8th April 2019), Site 2019 QA
SK 2 cover parts of Svidník and Stropkov Districts (EK provided GEO EYE 1
satellite image also from 8th April 2019, both SK 1 and SK 2 QA zones are
localised in East Slovakia). Site 2019 QA Sk 3 cover parts of Nitra, Šaľa and
Nové Zámky districts in the west part of Slovakia (EK provided World View 3
satellite image from 27th June 2019). The Satellite images were georeferenced by
SSCRI staff. Measured and archive control and check points were used. For all
54
three zones the Quality checks of georeference were carried out and control
protocol were elaborated.
Figure 5.15. Localization of the controlled sites in QA LPIS 2019.
Figure 5.16. Example of case with identified critical defect: a) Invalid perimeter of reference parcel
and b) Total absence of eligible features.
a
)
b
)
55
Figure 5.17. Example of the occurrence of non-agricultural land cover features on the reference
parcels with causes “Update“ – changes of the underlying land were not applied.
Figure 5.18. Example of the occurrence of non-agricultural land cover features on the reference
parcels with causes “Erroneous processing“ – a mistake of LPIS operator.
Remote sensing within crop yield and crop production forecasting (2018-2019)
Monitoring of Crop Conditions and Crop Monitoring
Regional monitoring of natural crop conditions aims to study the influence of
weather (coupled with soil) on crop growth and crop development during current
vegetation season.
NDVI (Normalized Difference Vegetation Index) are derived from NOAA’s
AVHRR sensor. The NDVI vegetation index, characterizes the total biomass state
(volume and vitality), the higher the NDVI value, the more biomass is developed
(characterized by a higher content of chlorophyll in plants and hence a more
potent photosynthesis) (Fig. 5.19).
56
Figure 5.19. Development of the NDVI vegetation index in 2019 and its comparison with the situation
in 2018 and long-term average. Data source: NPPC-VÚPOP.
Crop yield forecasting
The aim of the crop yield and crop production forecasting is to provide the
most likely, scientific, and as precise as possible independent forecast for main
agricultural crop yields for Ministry of Agriculture and Rural Development of the
Slovak Republic and for the public.
National Crop Yield and Crop Production Forecasting System has been created
on SSCRI and is based on three different principles which are applied to specify
vegetation indexes as biomass development stage and biomass development:
Remote Sensing method method of interpretation of vegetation indicators
(as NDVI or DMP Dry matter development) from satellite images
(mainly from low resolution satellite sensors as NOAA AVHRR and SPOT
Vegetation satellite system);
Bio-physical modelling (WOFOST model) and simulation of vegetation
indexes (mainly TWSO Total Dry Weight of Storage Organs and TAGP
Total Above Ground Production). In WOFOST, weather and
phenological data, soil hydro-physical data and crop physiological data are
utilized as model key inputs;
Integrated assessment method, which means the implementation of specific
meteorological and vegetation indicators in the statistical analysis, assesses
the impact of weather on the projected harvest. Integrated estimate
summarizes a wider range of disparate indicators and indices that are
57
currently for the purposes of forecasting yields and consequently the
production of crops used.
The crop yield and crop production forecasting is carried out for main
agricultural crops winter wheat, spring barley, oil seed rape, grain maize, sugar
beet, sunflower and potatoes. The forecasts are reported six times per year in
the half of May, June and July for “winter and spring crops” and in the end of
July, August and September for “summer crops”. The forecast results are
interpreted at national level as well as at NUTS3 and NUTS4 level. The example
of crop yield forecasting in 2019 can be seen in the Figs. 5.20a and 5.20b.
Figure 5.20. Example of crop yield forecasting with remote sensing in first decade of July in 2019 for
rape (a) and in the second decade of September for maize (b).
Verification of high resolution layer „HRL“ permanent grasslands for the
reference year 2015
Verification of the High Resolution Layer (HRL) of Permanent Grassland TTP
/ Grassland was conducted on NPPC VUPOP according to the current
methodology. „Guidelines for verification of High Resolution Layers produced
by the CLMS (Copernicus Land Monitoring Service) as part of the 2015 reference
year production“. Thematic accuracy assessment of the HRL Grassland layer is
the goal of verification. The HRL layers are provided by EEA to NPPC through
contract with Slovak Environmental Agency. The HRLs are part of the land
use/land cover mapping component of the Copernicus Land Monitoring Service
(CLMS), serving a broad user community from European public bodies to
Member States and regional environmental authorities, as well as the value-
adding sector. They provide support to various environmental policies and
political decision-making, and significantly contribute to assessing Europe’s
current environmental status and monitoring changes over time. The Pan-
European High Resolution Layers (HRL) provide information on specific land
cover characteristics, and are complementary to land cover / land use mapping
such as in the CORINE land cover (CLC) datasets. HRL -GRA is produced
20 a
58
primarily from Sentinels. The pan-European HRL 2015 Grassland Layer is
available at 20 m and 100 m resolutions. To achieve the 100 m map, an
aggregation process was carried out weighting grassland, non-grassland and
unclassifiable pixels at 20 m level within a 100 m grid cell. The class majority
determined the final assignment of the 100m grid cell to a specific class.
Verification was done by two methods: a general overview of HRL Grassland
data quality and using the "Look and Feel" method (for the recommended six
strata and two types of errors Commission and Omission). One type of “Omission
error” – is documented on Fig. 5.21 mostly grasslands without trees are correct
classified as permanent grassland. If part of the scattered trees is also presented
on agricultural land, some of them are not classified as HRL grassland TTP by
automatic classification of satellite images Sentinels. Example of Commission
error is showed on Fig. 5.22 arable land was classified as permanent grassland.
Relatively frequent error, especially if arable land and permanent grassland are
located side by side.
Verification was carried out visually in GIS environment interpretation and
comparison HRL Grassland with orthophotos and with thematic GIS layers
generated from the LPIS, biotopes of natural and semi-natural grassland and ZB
GIS. Generally, we conclude that the layer HRL permanent grassland is not well
classified. Time series of satellite images would help to improve the accuracy of
HRLs. In particular, various vegetation phases are a problem when identifying
Grasslands. In the future, data HRL Grassland are prerequisites for the use of data
and outcomes in a broader context.
Figure 5.21. „Omission error“ – Mostly grassland without scattered trees and bushes are classified
correct as HRL Grassland.
59
Figure 5.22. „Commission error“ arable land has been classified as permanent grassland TTP.
60
National Forest Centre Zvolen
Remote Sensing research activities of the National Forest Centre in Zvolen
were aimed at two main topics:
- Advanced Techniques for Biomass Mapping in Abandoned Agriculture Land
- Applications of airborne laser scanner technology in the forest management
Advanced Techniques for Biomass Mapping in Abandoned Agriculture Land
Abandonment of agricultural landscape is an all-European problem. In
Slovakia, this is a problem of large-scale land use in the area of 420-450 thousand.
ha, ie 17.5% 18.6% of the area of 2,423,478 ha of agricultural land. Wood
biomass outside forestland is not inventoried therefore information on the spatial
distribution, increment and volume of biomass on non-forest land is not available.
ATBIOMAP, the common project of the National Forest Centre and Institute
of Geography SAS supported by European Space Agency is aimed at mapping
and quantification of aboveground biomass on Abandoned Agricultural Land
(AAL).
Methodological framework is based on analyses and cross-validation of optical
(Sentinel 2) and radar satellite data (Sentinel 1 and ALOS PALSAR-2), supported
by field research and airborne laser scanning data (ALS). The project consists of
two main parts. In the first one (responsibility of the IG SAS), a classification
system for herbaceous, shrub and tree formations on AAL has been created and
included into a land cover (LC) mapping systems to contribute to tracking the
dynamics of AAL and its assessment. In the second part (responsibility of the
NFC), a mathematical model of biomass stock estimation and an innovative
methodology of permanent tree biomass inventory on AAL, based on satellite
data, has been developed. The models were derived and verified comparing
satellite biomass estimates and field data. A total of 104 plots (Fig. 5.23 and Fig.
5.24) were established to represent the full height growth range and heterogeneity
of the shrub and tree species composition on:
Study Area 1 Podunajská nížina, 39 plots, of which 33 scrubs (70% doge
rose dominated areas), 2 tree-like (Acer negundo) and 4 shrub-tree stands
(plums and nuts)
Study area 2 Zvolenská kotlina Víglaš: 65 plots, of which 30 scrubs
(blackthorn, dog rose), 25 forest stands (beech 28%, acacia 23%, cherry
12%, spruce 10%) and 10 shrub-tree stands
61
Figure 5.23. Field survey plots localisation in study area 1 Podunajská nížina (left) and study area
2 Zvolenská kotlina (right).
Figure 5.24. Left: field survey cut out of biomass from plot 2x2 m; Right: biomass weighing after
harvest using hanging scales.
Satellite data aquisition
Sentinel-1 satellite data were acquired from 5th September 2017 to 30th
September 2018
Sentinel-2 satellite data were acquired to 4 time periods: 22nd June 2016 (top
of vegetation season); 28th January 2017 (leaf-off vegetation season with
snow); 29th March 2017 (leaf-off vegetation season without snow) and 30th
September 2018 (autumn season).
Satelite radar ALOS-2 data we acquired in Stripmap mode (SLC format).
Study area 1: from 13th April 2017 (Northeast part) and 27th April 2017
(South-west part). Study area 2: 22nd April 2017.
Sentinel-1 processing include derivation of average intensity from both
polarisation VV and VH; Sigma0, Gamma0, Beta0 and applying Refined Lee
filter from 61 images acquired from 5th September 2017 to 30th September 2018.
62
Coherence between images were calculated from leaf-off periods: 14-20January
2017; 14-26January2017; 20-26January2017.
The aim of Sentinel-1 stratification was to analyse separately:
Leaf-on period (from 5.IX.2017 to 15.X.2017 and from 20.IV.2018 to
30.IX.2018)
Leaf-off period: 17.X.2017 19.IV.2018 with sub-stratum 1: Leaf-off period
without snow (from 17.X. to 14.XI.2017 and from 22.III. to 19.IV 2018) and
sub-stratum 2: Leaf-off period with snow (from 14.XI.2017 to 22.III.2018)
Sentinel-2 bands in the red, near and short-wavelength infrared regions were
included in the analysis, namely B4, B5, B8, B8a and B11 with a resolution of 10
and 20 m from all four periods. Topographically normalized images (L2A) were
used for all dates.
ALOS-2 data processing included derivation of backscatter sigma nought
(HH,VH,VV,HV), polarimetric parameters (Span, Pedestal Height, Radar
Vegetation Index, Radar Forest Degradation Index, Canopy Structure Index,
Volume Scattering Index, Biomass Index, Co and Cross Pol Ratio) and
polarimetric decomposition Sinclair and Pauli colour coding (Fig. 5.25),
Freeman-Durden, Sinclair, Yamaguchi and H/A/alfa decompositions (Fig. 5.26),
resp. Single bounce, Double bounce and Volume scattering layers. All relevant
products were also speckle filtered using Refined Lee approach.
Figure 5.25. Pauli combination of ALOS-2
satellite bands for test area Viglas, red HH-
VV green HV, blue HH+VV.
Figure 5.26. H/A/alfa decomposition for test area
Viglas Alfa parameter.
The extensive database allows derive many combinations of stock
prediction models on AAL (Tab. 5.1). We focused our attention on:
63
1) estimation of biomass volume on AAL from ALOS-2 bands applying
nonlinear (power) model,
2) fusion of Sentinel-1 and Sentinel-2 data and finding the most appropriate
methods for biomass volume prediction on AAL in 2 variants: linear and
nonlinear models of biomass estimation (Fig. 5.27),
3) Fusion of all disposable RS layers applying Random Forest Algorithm
(Fig. 5.28).
Table 5.1. Models for biomass retrieval on AAL for RS data
Inputs (bands)
Model backward stepwise multiple regression
AGB (t.ha-1)=
R2
RMSE
(t.ha-1)
Remark
ALOS-HV, HH
e(-5.75 + 5.10 * lnALOS_HV 3.12 * lnALOS_HH) * 1.51
0.63
117.9
ALOS-2
ALOS-VH, VV, HH, HV
-106.60 + 4.71 * ALOS-VH 3.19 * ALOS-HH
0.33
154.1
ALOS-2
Yamaguchi 1, Yama2, Yama3
-86.34 + 24.17 * yama2 - 23.45 * yama3
0.39
146.6
ALOS-2
Sinclair decomposition
-153.45 70.71 * sinc1 + 78.02 * sinc2
0.38
147,4
ALOS-2
Freeman decomposition
-54.45 + 21.64 * frem2 21.49 * frem3
0.38
147.7
ALOS-2
22.6.2016 (B4, B5,B8, B8a, B11)
730.71 - 0.79 * B5 1.62 * B8 + 1.47 * B8a
0.63
115.4
Sentinel-2
22.1.2017 (B4, B5,B8, B8a, B11)
295.66 + 0.43 * B8 0.51 * B8a + 0.17 * B11
0.36
151.2
Sentinel-2
29.3.2017 (B4, B5,B8, B8a, B11)
384.15 - 0.98 * B8 + 1.02 * B8a - 0.21 * B11
0.32
156.1
Sentinel-2
30.9.2018 (B4,B8, B11)
161.92 - 0.74 * B4 + 0.08 * B8
0.40
145.9
Sentinel-2
SNEH-VH0 VV0, VegO-VH0 VV0
-15.35 + 5.41 * SNEH-VH0 6.16 * VegO-VV0
0.37
148.8
Sentinel-1
SNEH-VH0-VV0, VegO-VH0-VV0,
Coherence VV-VH (14-20-26.I.2017)
179.68 - 3.65 * C2026iVV 4.37 * VegO-VV0 +
3.93 * SNEH-VH0
0.44
141.1
Sentinel-1
22.6.2016-B5, SNEH-VH, Veg-VV
544.61 - 0.54 * B5-22vi + 2.89 * S1-VHleaf-off -
3.38 * S1-VVleaf-on
0.58
100.1
Sentinel-1,2
Whole dataset
Random Forest Algorithm (in m3.ha-1)
0.75
106.8
All layers
Figure 5.27. Example of application of linear regression model (Sentinel-1,2) in the western part of
study area “Viglas”. Left – aerial scene, right raster of estimated biomass (tonnes per ha).
64
Figure 5.28. Predicted growing stock (m3/ha), Vígľaš test area, based on Random Forest
algorithm.
Applications of airborne laser scanner technology in the forest management
Remote sensing activities related to the airborne laser scanning (ALS) over the
years 2018-19 were solved based on research projects “Innovations in the forest
inventories based on progressive technologies of remote sensing” (APVV-15-
0393) and Research and development for support of the competitiveness of
Slovak forestry New methods of forest inventory based on combination of
terrestrial and aerial laser scanning” (SLOV-LES).
The main objective of all activities was an enhancement of the current inventory
methods based on more precise and economically effective combination of
different approaches (e.g. individual tree defection approach and area-based
approach) and different remote sensing data (e.g. combination of ALS data with
optical and/or radar data from terrestrial, aerial and satellite remote sensing
platform; Fig. 5.29).
The proposal of algorithm is implemented in reFLex (remote Forest Land
explorer) software and several studies already demonstrated that forest stand
variables can be estimated with sufficient accuracy using developed algorithm. A
Forest Management Unit Vígľaš covering a total area of 12,472 ha was selected
for assessment of accuracy and feasibility of developed algorithm. Specifically,
the differences between ground-measured and RS-estimated forest stands
variables reached values of 16.4%, 12.1%, −26.8%, and −35.4% for the mean
65
height, mean diameter, volume per hectare, and trees per hectare, respectively
(Sačkov et al. 2019a, 2019b).
Figure 5.29. Fusion of airborne (green colour) and terrestrial (blue colour) laser scanning data.
66
Ministry of Environment of the Slovak Republic (MOE SR)
Activities of the MOE SR were concentrated on the work involved with the
Copernicus programme:
Copernicus programme is the European programme for Earth Observation.
The Programme entered its full operational stage in the year 2014. The work on
the EU level was concentrated on cooperation with the Copernicus Committee,
Copernicus Security board, Copernicus User forum and Copernicus Ground
segment task force and commenting on the EU level the technical and legislative
documents regarding the Programme.
Cooperation with the European Space Agency (ESA) is limited due the fact
that the Slovak Republic is not full member of ESA yet. Slovakia is however
actively participating in Plan for European cooperating States (PECS). Several
organization and companies from Slovakia were successful in 5 open calls for
PECS projects. Cooperation with the European Environment Agency (EEA) was
concentrated on preparation of the next CORINE Land Cover (CLC) 2018 and
High Resolution Layer (HRL) products as a part of the Copernicus Land
observation service. At the national level the Slovak national Copernicus working
group continued its operation with the aim to coordinate Copernicus related
activities on the national level and dissemination of information related to
Copernicus programme. MOE SR distributes the Sentinel satellite images for the
Slovak Republic on demand. Compared to previous period user uptake and usage
of the Copernicus data has growing trend but is still relatively low compared to
neighbouring EU countries. Several public government organizations and private
companies are actively using Copernicus spatial data. In the following years
Slovakia plans to focus on user trainings in remote sensing and Programme
information dissemination.
Pavol Jozef Šafárik University in Košice is member of Copernicus academy
network and is actively using Copernicus programme spatial data in its courses
and lectures. Private company InSAR is successfully operate as member of
Copernicus Relays network, promoting the information about programme and
data usage to public and professional through workshops, courses and conference.
Two annual Hackathons were organised in Bratislava with successful use of the
Copernicus data by the participants to develop application prototypes.
67
Slovak Environmental Agency (SEA) in Banská Bystrica
Activities of the SEA were concentrated on the work involved with the
Copernicus programme:
Copernicus is the European programme for Earth Observation. The
Programme entered its full operational stage in the year 2014. The work on the
EU level was concentrated on cooperation with the Copernicus Committee,
Copernicus Security board, Copernicus User forum and Copernicus Ground
segment task force and commenting on the EU level the technical and legislative
documents regarding the Programme. Cooperation with the European Space
Agency is limited due the fact that the Slovak Republic is not full member of ESA
yet. Cooperation with the European Environment Agency (ESA) was
concentrated on implementation of the CORINE Land Cover (CLC) 2018 and the
High Resolution Layer (HRL) products as a part of the Copernicus Land
observation service. Copernicus supporting activities for the period 2017-2021:
Copernicus Land Monitoring
SEA joined the activities in project Copernicus Local Land monitoring services
under Framework Contract EEA/IDM/R0/16/009/Slovakia. The contract between
SEA and EEA was signed on 8 June 2017 and project tasks were implemented
from autumn 2017 till end of 2018. The project flagship was CLC2018, the fifth
CLC inventory in Europe. The final integrated European results are available
since late 2018.
Project tasks undertaken by SEA:
finalised in 2018-2019:
Verification of 2012 reference year local component products.
Production of CLC for the 2018 reference year.
Post-production verification of the HRLs for the 2015 reference year.
mapping national geospatial resources to EAGLE matrix
Post 2019 tasks:
Post-production verification of the HRLs for the 2018 reference year.
Support and testing of future CLC+ (2nd generation CLC
methodological improvements and developments), based on CLC2018
products.
68
Figure 5.30. The screenshot of new SEA webpage.
All of the time horizons CLC data has been published as standard OGC
services and also are available through new webpage http://corine.sazp.sk (Fig.
5.30). The info day about Corine Land Cover 2018 activities and output products
was also held on March, 28th, 2019 in SEA to fulfil project dissemination
activities.
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sensing control of area-based subsidies. Final report, NAFC-SSCRI Bratislava,
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surface urban heat island based on LANDSAT ETM+ and OLI/TIRS imagery in
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Detection Methods for Estimation of Forest Stand and Ecological Variables from
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6. SPACE METEOROLOGY 2018-2019
J. Kaňák, Ľ. Okon, L. Méri, M. Jurašek
6.1. Fully automated quantitative estimation of cloud top height using
stereoscopic Meteosat dual satellite observations
EUMETSAT provides perfect stereoscopic data from Meteosat 10/11 (Basic
service) and Meteosat 8 (IODC service) over large areas of Central and East
Europe, Middle East Asia, central and South African regions from 2016. The
presented work describes proposed experimental product, which is using AMV
(Atmospheric Motion Vectors algorithm) to detect mutual parallax shifts of
clouds in coupled imagery. This product is based on previous investigations of
manual measurements of parallax shifts, which were presented at the
EUMETSAT 2017 conference in Rome. Parallax shifts we are currently
calculating for 32x32 pixel boxes over 16x16 pixels grid, but are planned to be
tested also for smaller/optimized boxes and grid spacing. Fully automated
calculations over the big regions covered by dual satellites observations can serve
as important supplement data to other methods and products like NWCSAF Cloud
Top Height and Cloud Type, or shadows length based estimations of cloud top
heights. Algorithm is working not only with High Resolution Visible (HRV) but
also with other IR and VIS spectral bands. Considering 12 SEVIRI channels we
obtained wide experimental set of dual satellite parallax shifts for different cloud
types and heights. New, third generation of geostationary satellites with finer
image resolution and global coverage bring us to new possibilities how to
combine and use more efficiently overlapping satellite fields of view.
6.1.1. Mathematical background of automated quantitative estimation of
cloud top height
Fully automated computer processing of dual satellite images is divided in
SHMI operational chain into following steps:
1. Identification of cloud structures in the left and right satellite images using
Atmospheric Motion Vector (AMV) algorithm
2. Coupling cloud structures using dual set of Cartesian coordinates [xleft , yleft]
and [xright, yright]
3. Converting Cartesian to geographical coordinates [λleft , φleft] and [λright , φright]
4. Calculating parallax corrected positions of clouds in left and right image
[λleft , φleft]corr and [λright , φright]corr
5. Calculating horizontal (surface) distance d between left and right corrected
positions (note that for sea level parallax correction is equal to zero):
71
d = distance { [λleft , φleft]corr; [λright , φright]corr }
6. In iteration steps changing the elevation E in 100 meters steps from surface up
to 20 km atmosphere layer
7. Repeating calculation steps 3, 4, 5, 6 for each elevation E to look for minimal
horizontal distance dmin
8. Final statement of calculations: Elevation E(dmin) is corresponding to the
minimum distance dmin is considered as the height of the cloud.
Practical realization is done by numerical iteration process calculations of
the distance d between the lines connecting the satellite and the cloud finding
the height of minimum distance (intercept-point). Graphical explanation is shown
in Fig. 6.1.
Figure 6.1. Quantitative estimation of cloud top height using stereoscopic Meteosat dual satellite
observations. Iteration process is represented by set of horizontal yellow lines. Lines are representing
horizontal distance between left and right rays in different elevations. Minimum distance between lines
(in optimal case d=0) is indicating the cross point of these lines related to the cloud top height. In
practice zero value of d is only limit because of various sources of errors.
6.1.2. AMV (Atmospheric Motion Vectors) algorithm
Algorithm comes from CEI Nowcasting Project 2002-2004 in cooperation of
ZAMG Austria and SHMI Slovakia. Algorithm is based on definition of limited
area in the first image and look for identical image structure in the second image.
Shift of structure between images corresponds to mutual parallax shift between
left and right satellite cloud observations. Originally algorithm was used only for
WV channels smooth structures. We made set of tests with all infrared MSG
channels using standard cross-correlation technique applied to rectangular targets
72
over the image matrix with the aim of detecting optimal shift between target and
matcher.
Calculations are applied to regular satellite image grid (step size is optional from
maximum 10 to minimum single image pixels). Basic assumption must be
fulfilled that images from left and right satellites must be re-projected from Geo-
satellite view into common cartographic map. The core calculation expression is:
Software of this algorithm was originally written in Fotran-90. For the
purposes of automated quantitative estimation of cloud top height algorithm was
translated into C language and parametrized for optimal performance with image
data of MSG SEVIRI spectral bands as follows:
Parameter: Step 16x16 Step 8x8
Correlation window size 33 33
Span of possible displacements 36 36
X-coordinate of first column 32 32
Y-coordinate of first row 32 32
X-difference between vectors 16 8
Y-difference between vectors 16 8
Number of vectors in x-direction 122 244
Number of vectors in y-direction 91 182
Gaussian pyramid iterations 2 2
Number of smoothing cycles 3 3
6.1.3. Validation of proposed method and final product
AMV algorithm enables us to obtain quickly and automatically dual parallax
cloud shifts over the big regions monitored by dual MSG satellite constellation.
Output from the software is displayed in the special visualization tool, as it is
shown in Fig. 6.2. This tool can be used also for validation purposes, as the length
of arrows can be compared with manually measured parallax shifts and cloud top
can be derived; simultaneously we can use the tool to measure the length of cloud
shadows, which provide another way how to estimate cloud tops.
ii
ii
iii
yyxx
yyxx
r22 )()(
))((
max
73
Figure 6.2. Example shows the arrows, length of which is equivalent to Cloud Top Height (CTH).
Colour lines generated by validation tool represent directions to the left and right satellites. Cross points
of line couples are corresponding to the real cloud top position in 3-D coordinate system.
The most common problem occurring during validation was resulting from
improper or not accurate geolocation/rectification of satellite images. Precision of
geolocation depends on current satellite status of its positional sensors, which
provide auxiliary information for image rectification. As Meteosat-8 satellite was
launched in 2002, eccentricity of satellite axis rotation is much higher and we are
coupling the images from this satellite with Meteosat-10 or Meteosat-11, launched
in 2012 and 2015 respectively, with high rotational stability of their movement.
But using additional corrections of image rectification in case of Meteosat-8 we
were able to minimize errors of mutual parallax shifts. Results after these
corrections are showed in Fig. 6.3.
Final product is created using linear interpolation of gridded CTH data into
the original satellite grid. Example of final product is shown in Fig. 6.4.
Figure 6.3. Using additional correction of image rectification for Meteosat-8 we obtained proper
orientation of parallax shifts and more precise calculations of cloud tops.
74
Figure 6.4. Final Cloud Top Height product overlaid over the MSG satellite high resolution visible
image. Colour scale is calibrated in kilometres. Final precision of product according validation results
is 500 meters for 40% of cases and 1km for 60% of cases.
6.2. Way from MSG to MTG satellite user’s training and operational
supporting tools
6.2.1. Introduction
Geostationary satellites monitor practically the whole globe except Polar
Regions; therefore imagery from these satellites is very frequently used by
number of users over the world for weather and climate observations, and for
forecasting and nowcasting purposes. Different technical and software
capabilities are available through both commercial and non-commercial
opportunities for exploitation of these satellites in training and operational
activities. This work presents more than 10 years of skills with SHMI MSGProc
software development, distribution and communication with users who depend on
solutions based on simple installation, easy maintenance and minimum hardware
requirements. This kind of users was identified by EUMETSAT training division
in NMHS of south-east European region countries (so called DAWBEE users),
but also by our personal skills on the base of communication with users in Brazil,
Africa and other countries, mainly from the universities, where our software was
provided on the user’s request. This, originally MSG-dedicated software, is
currently renamed to “GEOProc” and enhanced to be reusable for new
geostationary platforms as HIMAWARI and GOES new generation with the
intention to be usable for Meteosat Third Generation (MTG) satellite imagery at
the first moment of MTG operations. We recognized openness of EUMETSAT in
this activity in the frame of ‘MTGUP!’ initiative.
75
6.2.2. Background
SHMI developed and is using operationally home-made processing software
for geo satellites, starting with MSG era:
MSGProc and new GEOProc for HIMAWARI, GOES-16, 17 data available
from EUMETCast system
New experiences thanks to close cooperation with EUMETSAT on DAWBEE
project (Data Access to West Balkan and East European countries)
The group of users was found, which requires easy to install, configure and
usage software for their needs
Opportunity to re-use current experience also for MTG satellite data
6.2.3. SHMI software solution
Some special features of SHMI solution are described and discussed in
presented work, starting with data acquisition, main processing steps up to final
RGB products generation and visualization. Attention is focused to effectiveness
of input data processing, data calibration, and special image corrections with
contribution of the Sun and satellite zenith angles, light diffusion in visible bands,
and anisotropy of atmosphere in infrared spectral bands. Considering that new
generation of geostationary satellites are providing much higher volumes of raw
data than current MSG satellites, we are now performing online data reception
tests via EUMETCast service from HIMAWARI-8, 9 and GOES-16, 17 satellites.
We also perform processing of these data to RGB imagery in operational mode.
First skills with the new software solution, and selected image examples of typical
weather situations from already generated list of products at SHMI are shown and
discussed in final part of this report.
6.2.4. Software concept and features
• Easy and quick installation
• Simple usage and maintenance
• Pre-defined RGB products are generated according well-known recipes
• New RGB products can be added easily or existing can be modified
• Effective usage of calculating resources and short processing time
Processing of current GEO (MSG, GOES, HIMAWARI) satellite
geostationary services
• C and C-shell programming without necessity of external libraries and third
party software
6.2.5 Corrections of solar channels
Because of increasing number of spectral bands parallel processing and reusing
of pre-calculated parameters approach was selected. Corrections of solar channels
76
are done for Sun height and Satellite zenith angles according functions shown in
Fig. 6.5.
Figure 6.5. Correction of solar albedo on Sun height (left) and on satellite zenith angle (right).
While Sun height is determined using standard Sun coordinates right
ascension and declination, functions for corrected albedo are based on empirical
equations (1).
Corr = 1./(a*sin(α)+b*sqrt(sn(α))); where a = 0.6 b = 0.4, α is Sun zenith angle (1)
offset_sunh ≈ pow ( MaxH - α, 3 ); partial correction offset for Sun height
offset_satz ≈ zenith / α; partial correction offset for Satellite zenith angle
offset = offset0 - offset_sunh - offset_satz; total correction offset
6.2.6 Airmass full Earth disk RGB enhanced
Originally set of RGB products was defined very early after the launch of the
first satellite from MSG satellite series. Product parameters (colour component’s
minimum and maximum values) were fixed over the whole Earth disk. After the
years EUMETSAT recommended to differentiate between equatorial and mid
latitudes for some RGB products, mainly when convection is displayed. We
suggested to use floating values instead of constants with the aim to put equatorial
and mid latitudes regions into common maps. Original settings for Airmass
product were:
Channel Min Max Gamma
Red Diff (6.2-7.3) -25° 1
Green Diff (9.6-11.2) -40° 1
Blue WV (6.2) 208K 243K -1
For the full disk containing also tropical regions we defined R, G, and B
thresholds depending on latitude according cosine shape as follows:
Channel Min Max Gamma
Red Diff (6.2-7.3) -25+Δ/2-Δcos (φ); Δ=-8 Min+25 1
Green Diff (9.6-11.2) -40+Δ/2-Δcos (φ); Δ=-8 Min+45 1
Blue WV (6.2) 208+Δ/2-Δcos (φ); Δ=20 Min+35 -1
Calculated new correction values for R, G and B components are shown in
Fig. 6.6.
77
Fig. 6.6. Latitude dependent minimum and maximum values of Airmass full Earth disk RGB
product color components; red at left up, green at upper right and blue at left down plot.
Processed full Earth disk image couple at right down: before (left) and after the correction
(right).
6.2.7. Selected demonstration cases and conclusions
Following list of meteorological cases was created for various scenes from
GOES and HIMAWARI imagery data:
Fire smoke and fire temp RGB products
Raikoke eruption and rotating SO2 clouds (Airmass wholes)
Goes-16 / MSG-4 comparison of common regions
Twin cyclones in Australia and Pacific
ship contrails GOES-16 2019-08-28 17:30 UTC
Sun eclipse in South America
Super typhoon Wutip of category 5 in western Pacific -10 minutes scan
EUMETCast Europe service of EUMETSAT is providing operationally
valuable data from new GEO satellites for training purposes of SHMU staff;
Thanks to this service users have opportunity monitor and study in (near) real
time weather over the globe;
Space and time of provided data is slightly reduced due to transfer capacities,
but good enough to make users familiar with new RGB possibilities based on new
set of 16 spectral channels (in comparison to old GEO standard 5 or 12 channels);
Users of new generation of EUMETSAT geo satellites must be aware in near
future that new channels and higher space and time resolution will bring extreme
requirements on data transfer and data processing; but they can await new
enhanced possibilities of new physical and meteorological information for
weather analyses and forecast.
78
6.3. Dual-frequency precipitation satellite radar and H-SAF product
upscaling procedure over MSG full-disk area developed at SHMI
Slovakia (SHMI) is member of consortium in EUMETSAT H-SAF project
since 2005. In cooperation with Italian Department of Civil Protection we are
cooperating in validation of satellite precipitation estimations. We are using
ground meteorological radar network data for standard validation of H-SAF
products over European region. But for global products like Precipitation rate at
ground by MW cross-track scanners (with indication of phase) it is more practical
to use other similar equipment on board of satellites. We found possibility of
validation using product 2ADPR Dual-frequency Precipitation Radar (DPR)
measurements on board of GPM (Global Precipitation Mission) satellites.
Example of such product is shown in Fig. 6.7.
Figure 6.7. Example of 2ADPR Precipitation Rate product based on measurements by DPR
instrument on board GPM satellites.
H-SAF product called H02B is a map of instantaneous precipitation (mm/hr)
generated from MW cross-track scanning radiometers on board of satellites in sun
synchronous orbit. Currently processing data are coming from AMSU-A/MHS on
board European MetOp and U.S. NOAA satellites. Spatial Resolution of product
corresponds to the nominal resolution of MHS, varying with the viewing scan
angle from 16 x 16 km2 (circular) at nadir to 26 x 52 km2 (ellipse) at scan edge.
According to user requirements the thresholds, target and optimal accuracy of
products is depending on precipitation range, as it is stated in the table:
Precipitation range
Threshold
Target
Optimal
> 10 mm/h
90
80
25
1-10 mm/h
120
105
50
< 1 mm/h
240
145
90
79
Example of H02B product is shown in Fig. 6.8.
Figure 6.8. Example of H02B product - instantaneous precipitation (mm/hr) generated from
MW cross-track scanning radiometers on board of satellites in sun synchronous orbit MetOp
(EUMETSAT) and NOAA.
To validate/compare these relatively different products we elaborated special
software package, which is re-mapping both products into common regular
longitude-latitude grid. Complete product set contains more parameters:
Cloud phase liquid-solid (discrete parameter)
Rate of product confidence (discrete parameter)
Land/Coast/Ocean flag (discrete parameter)
Precipitation rate mm/h (continuous parameter)
Standard deviation of precipitation rate (continuous parameter)
Time of acquisition in Julian day (continuous parameter)
Upscaling (re-mapping) of each parameter require different approach, which
depend on its characteristics. In general we split parameters to two categories
continuous and discrete. In upscaling algorithm mean value is selected for
continuous and median for discrete parameters. Visualized selected parameters
for H02 product are shown in Fig. 6.9, for 2DPR/GPM product in Fig. 6.10.
80
Figure 6.9. Upscale of H02B H-SAF product parameters to regular longitude-latitude grid in
resolution of 0.1x0.1 degrees. From left to the right: Land/Coast/Sea flag, Precipitation Rate,
Cloud Phase.
Figure 6.10. Upscale of 2DPR/GPM product parameters to regular longitude-latitude grid in
resolution of 0.1x0.1 degrees. From left to the right: Land/Coast/Sea flag, Precipitation Rate,
Cloud Phase.
H02B H-SAF product space resolution is lower, but the swath of satellite
instrument is quite wide, approximately 2250 km. In opposite, space resolution of
2ADPR/GPM product is higher, but swath of dual-frequency radar is much lower,
only 300 km. The advantage of 2ADPR product is that dual-frequency Doppler
radar is capturing precipitation intensities and phase with high reliability and
instrument data are physically better convertible to precipitation intensity than in
the case of microwave measurements with MetOp and NOAA satellites.
81
References:
[1] KAŇÁK, J. (2018). Fully automated quantitative estimation of cloud top
height using stereoscopic Meteosat satellite observations. EUMETSAT
Meteorological Satellite Conference. Tallin, 17.-21. September 2018.
https://www.eumetsat.int/website/wcm/idc/idcplg?IdcService=GET_FILE&dDo
cName=ZIP_CONF_2018_PRES_S3_ORAL&RevisionSelectionMethod=Lates
tReleased&Rendition=Web
[2] KUTIŠ, V., VALKO, P., DRŽÍK, M., SLAČKA, J., FARKAS, G., RAKÚS,
M., HUBINSKÝ, P., KAŇÁK, J. (2018). Kozmické technológie. Bratislava:
Slovenská technická univerzita.
[3] KAŇÁK, J., JURAŠEK, M., OKON, Ľ., MÉRI, L. (2019). Way from MSG to
MTG satellite user’s training and operational supporting tools. Joint
EUMETSAT/AMS/NOAA Conference. Boston, 30 September 4 October 2019.
Conference paper:
https://www.researchgate.net/publication/339301631_1E2_WAY_FROM_MSG
_TO_MTG_SATELLITE_USER'S_TRAINING_AND_OPERATIONAL_SUP
PORTING_TOOLS
Video-record from the coference:
https://ams.confex.com/ams/JOINTSATMET/videogateway.cgi/id/504859?reco
rdingid=504859
[4] PETRACCA, M., KAŇÁK, J., PORCU, F., IWANSKI, R., LAPETA, B.,
DIÓSZEGHY, M., SZENYÁN, I., BAGUIS, P., ROULIN, E., OZTOPAL, A.,
KRAHE, P., KUNKEL, A., ARTINIAN, E., ChERVENKOV, H.,
CACCIAMANI, C., TONIAZZO, A., VULPIANI, G., PUCA S. (2019). Results
of comparison between precipitation estimates by MW scanner and dual-
frequency precipitation satellite radar according H-SAF validation methodology
over MSG full-disk area. Joint EUMETSAT/AMS/NOAA Conference. Boston, 30
September 4 October 2019. Conference poster abstract link:
https://ams.confex.com/ams/JOINTSATMET/meetingapp.cgi/Paper/360562
82
7. INSTITUTIONS INVOLVED IN SPACE RESEARCH
Members of the National Committee of COSPAR with e-mail addresses.
The website of NC is http://nccospar.saske.sk.
Astronomical Institute (AI)
Slovak Academy of Sciences (SAS)
Stará Lesná
059 60 Tatranská Lomnica
J. Rybák (choc@astro.ta3.sk, NC member)
Faculty of Mathematics, Physics and Informatics (FMPI)
Comenius University
Mlynská dolina
842 15 Bratislava
J. Masarik (Jozef.Masarik@fmph.uniba.sk, NC member)
National Forest Centre
T.G. Masaryka 22
960 92 Zvolen
contact: T. Bucha (bucha@nlcsk.org)
Earth Science Institute (ESI)
Slovak Academy of Sciences (SAS)
Dúbravská cesta 9
840 05 Bratislava
M. Revallo (milos.revallo@savba.sk, Secretary of NC)
Institute of Animal Biochemistry and Genetics
Slovak Academy of Sciences (SAS)
Moyzesova 61
900 28 Ivanka pri Dunaji
I. Hapala (Ivan.Hapala@savba.sk, NC member)
Institute of Experimental Endocrinology (IEE)
Slovak Academy of Sciences (SAS)
Vlárska 3
833 06 Bratislava
83
Institute of Experimental Physics (IEP)
Slovak Academy of Sciences (SAS)
Watsonova 47
040 01 Košice
P. Bobík (bobik@saske.sk, NC member)
Institute of Geography (IGG)
Slovak Academy of Sciences (SAS)
Štefánikova 49
814 73 Bratislava
J. Feranec (feranec@savba.sk, Vice-Chair of NC)
Institute of Materials and Machine Mechanics
Slovak Academy of Sciences (SAS)
Račianska 75
831 02 Bratislava 3
J. Lapin (juraj.lapin@savba.sk, NC member)
Institute of Measurement Science (IMS)
Slovak Academy of Sciences (SAS)
Dúbravská 9
842 19 Bratislava
contact: I. Frollo (frollo@savba.sk)
Institute of Normal and Pathological Physiology (INPP)
Slovak Academy of Sciences (SAS)
Sienkiewiczova 1
813 71 Bratislava
contact: F. Hlavačka (Frantisek.Hlavacka@savba.sk)
Slovak Central Observatory (SCO)
Komárňanská 137
947 01 Hurbanovo
I. Dorotovič (ivan.dorotovic@suh.sk, Chair of NC, Representative
of Slovak NC to COSPAR)
Ministry of Environment of the Slovak Republic
Tajovského 28
975 90 Banská Bystrica
contact: J. Nováček (jozef.novacek@enviro.gov.sk)
84
Slovak Hydrometeorological Institute
Jeséniova 17
833 15 Bratislava
contact: J. Kaňák (jan.kanak@shmu.sk, NC member)
Slovak Organization for Space Activities (SOSA)
Ilkovičova 3 (FEI STU)
812 19 Bratislava
contact: M. Musilová (michaela.musilova@stuba.sk, NC member)
National Agricultural and Food Centre
Soil Science and Conservation Research Institute
Trenčianska 55
821 09 Bratislava
contact: M. Sviček (michal.svicek@nppc.sk)
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